45 results on '"Gregory A. Feiden"'
Search Results
2. TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System
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Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, and Chelsea X. Huang
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Stellar ages ,Transit photometry ,Exoplanets ,Stellar associations ,Stellar kinematics ,Astronomy ,QB1-991 - Abstract
We report the discovery and characterization of a nearby (∼85 pc), older (27 ± 3 Myr), distributed stellar population near Lower Centaurus Crux (LCC), initially identified by searching for stars comoving with a candidate transiting planet from TESS (HD 109833; TOI 1097). We determine the association membership using Gaia kinematics, color–magnitude information, and rotation periods of candidate members. We measure its age using isochrones, gyrochronology, and Li depletion. While the association is near known populations of LCC, we find that it is older than any previously found LCC subgroup (10–16 Myr), and distinct in both position and velocity. In addition to the candidate planets around HD 109833, the association contains four directly imaged planetary-mass companions around three stars, YSES-1, YSES-2, and HD 95086, all of which were previously assigned membership in the younger LCC. Using the Notch pipeline, we identify a second candidate transiting planet around HD 109833. We use a suite of ground-based follow-up observations to validate the two transit signals as planetary in nature. HD 109833 b and c join the small but growing population of
- Published
- 2023
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3. A Stringent Test of Magnetic Models of Stellar Evolution
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Guillermo Torres, Gregory A. Feiden, Andrew Vanderburg, and Jason L. Curtis
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stellar evolution ,eclipsing binaries ,fundamental stellar parameters ,stellar activity ,magnetic fields ,open clusters ,Astronomy ,QB1-991 - Abstract
Main-sequence stars with convective envelopes often appear larger and cooler than predicted by standard models of stellar evolution for their measured masses. This is believed to be caused by stellar activity. In a recent study, accurate measurements were published for the K-type components of the 1.62-day detached eclipsing binary EPIC 219511354, showing the radii and temperatures for both stars to be affected by these discrepancies. This is a rare example of a system in which the age and chemical composition are known, by virtue of being a member of the well-studied open cluster Ruprecht 147 (age~3 Gyr, [Fe/H] = +0.10). Here, we report a detailed study of this system with nonstandard models incorporating magnetic inhibition of convection. We show that these calculations are able to reproduce the observations largely within their uncertainties, providing robust estimates of the strength of the magnetic fields on both stars: 1600 ± 130 G and 1830 ± 150 G for the primary and secondary, respectively. Empirical estimates of the magnetic field strengths based on the measured X-ray luminosity of the system are roughly consistent with these predictions, supporting this mechanism as a possible explanation for the radius and temperature discrepancies.
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- 2021
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4. The TIME Table: rotation and ages of cool exoplanet host stars
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Eric Gaidos, Zachary Claytor, Ryan Dungee, Aleezah Ali, and Gregory A Feiden
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Earth and Planetary Astrophysics (astro-ph.EP) ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,FOS: Physical sciences ,Astronomy and Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Age is a stellar parameter that is both fundamental and difficult to determine. Among middle-aged M dwarfs, the most prolific hosts of close-in and detectable exoplanets, gyrochronology is the most promising method to assign ages, but requires calibration by rotation-temperature sequences (gyrochrones) in clusters of known ages. We curated a catalog of 249 late K- and M-type (($T_{eff}$=3200-4200K) exoplanet host stars with established rotation periods, and applied empirical, temperature-dependent rotation-age relations based on relevant published gyrochrones, including one derived from observations of the 4 Gyr-old open cluster M67. We estimated ages for 227 of these stars, and upper limits for 8 others, excluding 14 which have too rapidly rotating or are otherwise outside the valid parameter range of our gyrochronology. We estimated uncertainties based on observed scatter in rotation periods in young clusters, error in the gyrochrones, and uncertainties in temperature and non-solar metallicity. For those stars with measured metallicities, we provide but do not incorporate a correction for the effects of deviation from solar metallicity. The age distribution of our sample declines to near zero at 10 Gyr, the age of the Galactic disk, with the handful of outliers explainable by large uncertainties. Continued addition or extension of cluster rotation sequences to more thoroughly calibrate the gyrochronology in time and temperature space, more precise and robust measurement of rotation periods, and more accurate stellar parameter measurements will enable continued improvements in the age estimates of these important exoplanet host stars., accepted to MNRAS. Full Table 1 in CDS machine-readable format included as ancillary file time_table.mrt
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- 2023
5. TESS Hunt for Young and Maturing Exoplanets (THYME) IX: a 27 Myr extended population of Lower-Centaurus Crux with a transiting two-planet system
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Mackenna L. Wood, Andrew W. Mann, Madyson G. Barber, Jonathan L. Bush, Adam L. Kraus, Benjamin M. Tofflemire, Andrew Vanderburg, Elisabeth R. Newton, Gregory A. Feiden, George Zhou, Luke G. Bouma, Samuel N. Quinn, David J. Armstrong, Ares Osborn, Vardan Adibekyan, Elisa Delgado Mena, Sergio G. Sousa, Jonathan Gagné, Matthew J. Fields, Reilly P. Milburn, Pa Chia Thao, Stephen P. Schmidt, Crystal L. Gnilka, Steve B. Howell, Nicholas M. Law, Carl Ziegler, César Briceño, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Joshua E. Schlieder, Hugh P. Osborn, Joseph D. Twicken, David R. Ciardi, and Chelsea X. Huang
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Earth and Planetary Astrophysics (astro-ph.EP) ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,FOS: Physical sciences ,Astronomy and Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery and characterization of a nearby (~ 85 pc), older (27 +/- 3 Myr), distributed stellar population near Lower-Centaurus-Crux (LCC), initially identified by searching for stars co-moving with a candidate transiting planet from TESS (HD 109833; TOI 1097). We determine the association membership using Gaia kinematics, color-magnitude information, and rotation periods of candidate members. We measure it's age using isochrones, gyrochronology, and Li depletion. While the association is near known populations of LCC, we find that it is older than any previously found LCC sub-group (10-16 Myr), and distinct in both position and velocity. In addition to the candidate planets around HD 109833 the association contains four directly-imaged planetary-mass companions around 3 stars, YSES-1, YSES-2, and HD 95086, all of which were previously assigned membership in the younger LCC. Using the Notch pipeline, we identify a second candidate transiting planet around HD 109833. We use a suite of ground-based follow-up observations to validate the two transit signals as planetary in nature. HD 109833 b and c join the small but growing population of, 23 pages, 15 figures, Accepted for publication in AJ
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- 2022
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6. Gaia Gaps and the Physics of Low-Mass Stars. I. The Fully Convective Boundary
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Wei-Chun Jao, Khian Skidmore, and Gregory A. Feiden
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010504 meteorology & atmospheric sciences ,Stellar population ,Hertzsprung–Russell diagram ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Instability ,symbols.namesake ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Stellar evolution ,Astrophysics::Galaxy Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,0105 earth and related environmental sciences ,Physics ,Star formation ,Diagram ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,symbols ,Astrophysics::Earth and Planetary Astrophysics ,Low Mass - Abstract
The Gaia M-dwarf gap is a significant under-density of stars observed near $M_G = 10.2$ in a color-magnitude diagram for stars within 200 pc of the Sun. It has been proposed that the gap is the manifestation of structural instabilities within stellar interiors due to non-equilibrium $^{3}$He fusion prior to some stars becoming fully convective. To test this hypothesis, we use Dartmouth stellar evolution models, MARCS model atmospheres, and simple stellar population synthesis to create synthetic $M_G$-($G_{\rm BP} - G_{\rm RP})$ color-magnitude diagrams. We confirm that the proposed $^{3}$He instability is responsible for the appearance of the M-dwarf gap. Our synthetic gap shows qualitatively similar features to the observed gap including: its vertical extent in $M_G$, its slope in the color-magnitude diagram, and its relative prominence at bluer colors as compared to redder colors. Furthermore, corresponding over-densities of stars above the gap are reproduced by the models. While qualitatively similar, the synthetic gap is approximately 0.2 magnitudes bluer and, accounting for this color offset, 0.16 magnitudes brighter than the observed gap. Our results reveal that the Gaia M dwarf gap is sensitive to conditions within cores of M dwarf stars, making the gap a powerful tool for testing the physics of M dwarf stars and potentially using M dwarfs to understand the local star formation history., Comment: 20 pages, 8 figures, accepted for publication in ApJ, comments welcome
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- 2020
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7. An Enhanced Hertzsprung–Russell Diagram Using Gaia EDR3 Data
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Gregory A. Feiden and Wei-Chun Jao
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symbols.namesake ,Hertzsprung–Russell diagram ,Computer science ,symbols ,General Medicine ,Astrophysics - Published
- 2021
8. TESS Hunt for Young and Maturing Exoplanets (THYME): A Planet in the 45 Myr Tucana–Horologium Association
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Jon M. Jenkins, Steven Villeneuva, Mackenna L. Wood, Coel Hellier, Luke G. Bouma, John F. Kielkopf, Sara Seager, Jason J. Wang, Joseph E. Rodriguez, Christopher J. Burke, Thomas Barclay, Raquel A. Martinez, Joel Villasenor, Robert L. Morris, Adam L. Kraus, Pa Chia Thao, Gregory A. Feiden, Andrew W. Mann, Karen A. Collins, Eric L. Nielsen, Andrew Vanderburg, Robert J. De Rosa, Robert A. Wittenmyer, Misty Davies, Matthew W. Mengel, Jie Li, Chris Stockdale, Jack Okumura, Aaron C. Rizzuto, Logan A. Pearce, Jack J. Lissauer, David W. Latham, Rhodes Hart, Joshua N. Winn, Bruce Macintosh, Duncan J. Wright, Diana Dragomir, Koji Mukai, Rayna Rampalli, George R. Ricker, F. Mallia, Marshall C. Johnson, David R. Anderson, Jean-Baptiste Ruffio, Roland Vanderspek, Carolyn Brown, Peter F. Nelson, Giovanni Isopi, Benjamin M. Tofflemire, Ian A. Waite, Elisabeth R. Newton, and Michael Fausnaugh
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010504 meteorology & atmospheric sciences ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Photometry (optics) ,Neptune ,Planet ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Visual binary ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Astronomy and Astrophysics ,Planetary system ,Orbital period ,Exoplanet ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,QB799 - Abstract
Young exoplanets are snapshots of the planetary evolution process. Planets that orbit stars in young associations are particularly important because the age of the planetary system is well constrained. We present the discovery of a transiting planet larger than Neptune but smaller than Saturn in the 45 Myr Tucana-Horologium young moving group. The host star is a visual binary, and our follow-up observations demonstrate that the planet orbits the G6V primary component, DS Tuc A (HD 222259A, TIC 410214986). We first identified transits using photometry from the Transiting Exoplanet Survey Satellite (TESS; alerted as TOI 200.01). We validated the planet and improved the stellar parameters using a suite of new and archival data, including spectra from SOAR/Goodman, SALT/HRS and LCO/NRES; transit photometry from Spitzer; and deep adaptive optics imaging from Gemini/GPI. No additional stellar or planetary signals are seen in the data. We measured the planetary parameters by simultaneously modeling the photometry with a transit model and a Gaussian process to account for stellar variability. We determined that the planetary radius is $5.70\pm0.17$ Earth radii and that the orbital period is 8.1 days. The inclination angles of the host star's spin axis, the planet's orbital axis, and the visual binary's orbital axis are aligned within 15 degrees to within the uncertainties of the relevant data. DS Tuc Ab is bright enough (V=8.5) for detailed characterization using radial velocities and transmission spectroscopy., Accepted to ApJ Letters 2019 June 11
- Published
- 2019
9. How to Constrain Your M Dwarf. II. The Mass–Luminosity–Metallicity Relation from 0.075 to 0.70 Solar Masse
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Pa Chia Thao, Megan Ansdell, Adam L. Kraus, Jason Dittmann, Raquel A. Martinez, Samuel Factor, Gregory A. Feiden, Dary Ruíz-Rodríguez, Trent J. Dupuy, Michael J. Ireland, Eric Gaidos, Chao-Ling Hung, Aaron C. Rizzuto, and Andrew W. Mann
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Physics ,Solar mass ,astro-ph.SR ,Space and Planetary Science ,Metallicity ,Astronomy and Astrophysics ,Astrophysics ,Luminosity - Abstract
The mass–luminosity relation for late-type stars has long been a critical tool for estimating stellar masses. However, there is growing need for both a higher-precision relation and a better understanding of systematic effects (e.g., metallicity). Here we present an empirical relationship between M K and M * spanning 0.075 M ⊙ < M * < 0.70 M ⊙. The relation is derived from 62 nearby binaries, whose orbits we determine using a combination of Keck/NIRC2 imaging, archival adaptive optics data, and literature astrometry. From their orbital parameters, we determine the total mass of each system, with a precision better than 1% in the best cases. We use these total masses, in combination with resolved K S magnitudes and system parallaxes, to calibrate the M K–M * relation. The resulting posteriors can be used to determine masses of single stars with a precision of 2%–3%, which we confirm by testing the relation on stars with individual dynamical masses from the literature. The precision is limited by scatter around the best-fit relation beyond measured M * uncertainties, perhaps driven by intrinsic variation in the M K–M * relation or underestimated uncertainties in the input parallaxes. We find that the effect of [Fe/H] on the M K–M * relation is likely negligible for metallicities in the solar neighborhood (0.0% ± 2.2% change in mass per dex change in [Fe/H]). This weak effect is consistent with predictions from the Dartmouth Stellar Evolution Database, but inconsistent with those from MESA Isochrones and Stellar Tracks (at 5σ). A sample of binaries with a wider range of abundances will be required to discern the importance of metallicity in extreme populations (e.g., in the Galactic halo or thick disk).
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- 2019
10. Masses and Implications for Ages of Low-Mass Pre-Main Sequence Stars in Taurus and Ophiuchus
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Gail Schaefer, Vincent Piétu, E. Chapillon, Nicolas Grosso, Stephane Guilloteau, E. Di Folco, Anne Dutrey, Tracy L. Beck, Lisa Prato, Gregory A. Feiden, Michal Simon, Departement of Physics and Astronomy [SUNY], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), Departement of Astrophysics, American Museum of Natural History, NY, American Museum of Natural History (AMNH), AMOR 2019, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
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010504 meteorology & atmospheric sciences ,Hertzsprung–Russell diagram ,[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,symbols.namesake ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Physics ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Exoplanet ,Magnetic field ,Stars ,T Tauri star ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Ophiuchus ,symbols ,Astrophysics::Earth and Planetary Astrophysics ,Low Mass ,Main sequence - Abstract
The accuracy of masses of pre-main sequence (PMS) stars derived from their locations on the Hertzsprung-Russell Diagram (HRD) can be tested by comparison with accurate and precise masses determined independently. We present 29 single stars in the Taurus star-forming region (SFR) and 3 in the Ophiuchus SFR with masses measured dynamically to a precision of at least $10 \%$. Our results include 9 updated mass determinations and 3 that have not had their dynamical masses published before. This list of stars with fundamental, dynamical masses, M$_{dyn}$, is drawn from a larger list of 39 targets in the Taurus SFR and 6 in the Ophiuchus SFR. Placing the stars with accurate and precise dynamical masses on HRDs that do not include internal magnetic fields underestimates the mass compared to M$_{dyn}$ by about $30 \%$. Placing them on an HRD that does include magnetic fields yields mass estimates in much better agreement with M$_{dyn}$, with an average difference between M$_{dyn}$ and the estimated track mass of $0.01\pm0.02$~\msun. The ages of the stars, 3--10 MY on tracks that include magnetic fields, is older than the 1--3 MY indicated by the non-magnetic models. The older ages of T Tauri stars predicted by the magnetic models increase the time available for evolution of their disks and formation of the giant gas exoplanets. The agreement between our M$_{dyn}$ values and the masses on the magnetic field tracks provides indirect support for these older ages., Ap.J. to be published
- Published
- 2019
11. Stellar Evolution Models of Young Stars: Progress and Limitations
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Gregory A. Feiden
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010308 nuclear & particles physics ,Computer science ,Starspot ,FOS: Physical sciences ,Astronomy ,Astronomy and Astrophysics ,01 natural sciences ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Young star ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,010303 astronomy & astrophysics ,Stellar evolution ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics - Abstract
Stellar evolution models are a cornerstone of young star astrophysics, which necessitates that they yield accurate and reliable predictions of stellar properties. Here, I review the current performance of stellar evolution models against young astrophysical benchmarks and highlight recent progress incorporating non-standard physics, such as magnetic field and starspots, to explain observed deficiencies. While addition of these physical processes leads to improved agreement between models and observations, there are several fundamental limitations in our understanding about how these physical processes operate. These limitations inhibit our ability to form a coherent picture of the essential physics needed to accurately compute young stellar models, but provide rich avenues for further exploration., Comment: 6 pages, 1 figure, to appear in proceedings of IAU Symposium 314: Young Stars and Planets Near the Sun
- Published
- 2015
12. Fine Structures in the Main Sequence Revealed by Gaia Data Release 2
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Gregory A. Feiden and Wei-Chun Jao
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Physics ,Space and Planetary Science ,Astronomy and Astrophysics ,Biological system ,Data release ,Sequence (medicine) - Published
- 2020
13. The blue straggler V106 in NGC6791: A prototype progenitor of old single giants masquerading as young
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S. Meibom, Imants Platais, Torben Arentoft, Robert G. Izzard, Gregory A. Feiden, Frank Grundahl, H. Bruntt, Matthew Shetrone, Jens Jessen-Hansen, Thomas M. Tauris, Dennis Stello, S. Frandsen, K. Brogaard, Jerome A. Orosz, Andrea Miglio, Nils Ryde, Robert D. Mathieu, Don A. VandenBerg, Aaron M. Geller, Eric L. Sandquist, and S. M. Christiansen
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Physics ,close [binaries] ,010308 nuclear & particles physics ,Red giant ,fundamental parameters [stars] ,White dwarf ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Orbital period ,01 natural sciences ,Blue straggler ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,individual: V106 [stars] ,blue stragglers ,0103 physical sciences ,Binary star ,Low Mass ,010303 astronomy & astrophysics ,Stellar evolution ,Solar and Stellar Astrophysics (astro-ph.SR) ,Open cluster ,white dwarfs - Abstract
We determine the properties of the binary star V106 in the old open cluster NGC6791. We identify the system to be a blue straggler cluster member by using a combination of ground-based and Kepler photometry and multi-epoch spectroscopy. The properties of the primary component are found to be $M_{\rm p}\sim1.67 \rm M_{\odot}$, more massive than the cluster turn-off, with $R_{\rm p}\sim1.91 \rm R_{\odot}$ and $T_{\rm eff}=7110\pm100$ K. The secondary component is highly oversized and overluminous for its low mass with $M_{\rm s}\sim0.182 \rm M_{\odot}$, $R_{\rm s}\sim0.864 \rm R_{\odot}$ and $T_{\rm eff}=6875\pm200$ K. We identify this secondary star as a bloated (proto) extremely low-mass helium white dwarf. These properties of V106 suggest that it represents a typical Algol-paradox system and that it evolved through a mass-transfer phase which provides insight into its past evolution. We present a detailed binary stellar evolution model for the formation of V106 using the MESA code and find that the mass-transfer phase only ceased about 40 Myr ago. Due to the short orbital period (P=1.4463 d) another mass-transfer phase is unavoidable once the current primary star evolves towards the red giant phase. We argue that V106 will evolve through a common-envelope phase within the next 100 Myr and merge to become a single over-massive giant. The high mass will make it appear young for its true age, which is revealed by the cluster properties. Therefore, V106 is potentially a prototype progenitor of old field giants masquerading as young., Comment: 12 pages, 7 figures, accepted for publication in MNRAS
- Published
- 2018
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14. The Factory and the Beehive. III. PTFEB132.707+19.810, A Low-mass Eclipsing Binary in Praesepe Observed by PTF and K2
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Howard Isaacson, Adam L. Kraus, Marcel A. Agüeros, Kevin R. Covey, Andrew W. Howard, Gáspár Á. Bakos, Nicholas M. Law, Aaron C. Rizzuto, Gregory A. Feiden, Stephanie T. Douglas, Eric Gaidos, Guillermo Torres, and Andrew W. Mann
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Physics ,010504 meteorology & atmospheric sciences ,Metallicity ,Starspot ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Radius ,01 natural sciences ,Tidal locking ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Limb darkening ,0103 physical sciences ,Low Mass ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,0105 earth and related environmental sciences ,Commensurability (astronomy) - Abstract
Theoretical models of stars constitute a fundamental bedrock upon which much of astrophysics is built, but large swaths of model parameter space remain uncalibrated by observations. The best calibrators are eclipsing binaries in clusters, allowing measurement of masses, radii, luminosities, and temperatures, for stars of known metallicity and age. We present the discovery and detailed characterization of PTFEB132.707+19.810, a P=6.0 day eclipsing binary in the Praesepe cluster ($��$~600--800 Myr; [Fe/H]=0.14$\pm$0.04). The system contains two late-type stars (SpT$_P$=M3.5$\pm$0.2; SpT$_S$=M4.3$\pm$0.7) with precise masses ($M_p=0.3953\pm0.0020$~$M_{\odot}$; $M_s=0.2098\pm0.0014$~$M_{\odot}$) and radii ($R_p=0.363\pm0.008$~$R_{\odot}$; $R_s=0.272\pm0.012$~$R_{\odot}$). Neither star meets the predictions of stellar evolutionary models. The primary has the expected radius, but is cooler and less luminous, while the secondary has the expected luminosity, but is cooler and substantially larger (by 20%). The system is not tidally locked or circularized. Exploiting a fortuitous 4:5 commensurability between $P_{orb}$ and $P_{rot,prim}$, we demonstrate that fitting errors from the unknown spot configuration only change the inferred radii by, Accepted to ApJ; 36 pages, 19 figures, 8 tables in two-column AASTEX6 format
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- 2017
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15. Age of the magnetically active WW Psa and TX Psa members of the beta Pictoris association
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Thiam-Guan Tan, P. Elliott, A. Buccino, R. Petrucci, Gregory A. Feiden, E. Jofre, Pablo J. D. Mauas, R. Santallo, and Sergio Messina
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Physics ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,STARSPOTS ,Astrophysics ,LATE-TYPE [STARS] ,01 natural sciences ,Stars ,LOW-MASS [STARS] ,Space and Planetary Science ,0103 physical sciences ,Beta Pictoris ,GENERAL [BINARIES] ,ACTIVITY [STARS] ,Association (psychology) ,010303 astronomy & astrophysics - Abstract
There are a variety of different techniques available to estimate the ages of pre-main-sequence stars. Components of physical pairs, thanks to their strict coevality and the mass difference, such as the binary system analyzed in this paper, are best suited to test the effectiveness of these different techniques. We consider the system WW Psa + TX Psa whose membership of the 25-Myr β Pictoris association has been well established by earlier works. We aim to investigate which age-dating technique provides the best agreement between the age of the system and that of the association. Methods. We have photometrically monitored WW Psa and TX Psa and measured their rotation periods as P = 2.37 d and P = 1.086 d, respectively. We have retrieved their Li equivalent widths from the literature and measured their effective temperatures and luminosities. We investigated whether the ages of these stars derived using three independent techniques, that is based on rotation, Li equivalent widths, and the position in the HR diagram are consistent with the age of the β Pictoris association. We find that the rotation periods and the Li contents of both stars are consistent with the distribution of other bona fide members of the cluster. On the contrary, the isochronal fitting provides similar ages for both stars, but a factor of about four younger than the quoted age of the association, or about 30% younger when the effects of magnetic fields are included. Conclusions. We explore the origin of the discrepant age inferred from isochronal fitting, including the possibilities that either the two components may be unresolved binaries or that the basic stellar parameters of both components are altered by enhanced magnetic activity. The latter is found to be the more reasonable cause, suggesting that age estimates based on Li content are more reliable than isochronal fitting for pre-main-sequence stars with pronounced magnetic activity. Fil: Messina, S.. Inaf-catania Astrophysical Observatory; Italia Fil: Santallo, R.. Southern Stars Observatory; Polinesia Francesa Fil: Tan, T. G.. Perth Exoplanet Survey Telescope; Australia Fil: Elliott, P.. European Southern Observatory; Chile. University of Exeter; Reino Unido Fil: Feiden, G. A.. Uppsala University. Department Of Physics And Astronomy; Suecia Fil: Buccino, Andrea Paola. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Mauas, Pablo Jacobo David. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Petrucci, Romina Paola. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Departamento de Astrofísica Estelar; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina Fil: Jofre, Jorge Emiliano. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Departamento de Astrofísica Estelar; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina
- Published
- 2017
16. Magnetic field induced radius inflation of low-mass stars
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Gregory A. Feiden and Brian Chaboyer
- Subjects
Inflation (cosmology) ,Physics ,Metallicity ,General Engineering ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Radius ,Magnetic field ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Radiative transfer ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Low Mass ,Stellar evolution ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics - Abstract
We present results obtained using the magnetic Dartmouth stellar evolution code that address the possibility that magnetic fields are inflating low-mass stars in detached eclipsing binaries. While it seems plausible that magnetic fields are inflating stars with radiative cores, the level of inflation observed among fully convective stars appears too large to be explained by magnetic fields. We provide an alternative explanation, stellar metallicity, and propose observations that can help further constrain stellar models., Comment: 4 pages, 3 figures, to appear in proceedings from "Binary 2013: Setting a new standard in the analysis of binary stars."
- Published
- 2013
17. Zodiacal Exoplanets in Time (ZEIT) II. A 'Super-Earth' Orbiting a Young K Dwarf in the Pleiades Neighborhood
- Author
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James R. Graham, Megan Ansdell, Daniel T. Jaffe, Gregory A. Feiden, Eric Gaidos, Yoichi Takeda, Teriyuki Hirano, Aaron C. Rizzuto, Andrew W. Mann, Thomas M. Esposito, Larissa Nofi, Norio Narita, Gregory N. Mace, Adam L. Kraus, R. J. De Rosa, and Andrew Vanderburg
- Subjects
Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Dwarf star ,Super-Earth ,Zodiacal light ,010308 nuclear & particles physics ,Astronomy ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Planetary system ,Star (graph theory) ,01 natural sciences ,Exoplanet ,13. Climate action ,Space and Planetary Science ,Planet ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Pleiades ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We describe a "super-Earth"-size ($2.30\pm0.15R_{\oplus}$) planet transiting an early K-type dwarf star in the Campaign 4 field observed by the K2 mission. The host star, EPIC 210363145, was identified as a member of the approximately 120-Myr-old Pleiades cluster based on its kinematics and photometric distance. It is rotationally variable and exhibits near-ultraviolet emission consistent with a Pleiades age, but its rotational period is ~20 d and its spectrum contains no H$��$ emission nor the Li I absorption expected of Pleiades K dwarfs. Instead, the star is probably an interloper that is unaffiliated with the cluster, but younger (< 1 Gyr) than the typical field dwarf. We ruled out a false positive transit signal produced by confusion with a background eclipsing binary by adaptive optics imaging and a statistical calculation. Doppler radial velocity measurements limit the companion mass to, submitted to MNRAS, comments welcome
- Published
- 2016
18. Magnetic Inhibition of Convection and the Fundamental Properties of Low-Mass Stars. III. A Consistent 10 Myr Age for the Upper Scorpius OB Association
- Author
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Gregory A. Feiden
- Subjects
Convection ,Stellar mass ,Hertzsprung–Russell diagram ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Stellar classification ,01 natural sciences ,symbols.namesake ,0103 physical sciences ,Radiative transfer ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Stellar evolution ,Astrophysics::Galaxy Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Physics ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,symbols ,Astrophysics::Earth and Planetary Astrophysics ,Low Mass ,human activities - Abstract
When determining absolute ages of identifiably young stellar populations, results strongly depend on which stars are studied. Cooler (K, M) stars typically yield ages that are systematically younger than warmer (A, F, G) stars by a factor of two. I explore the possibility that these age discrepancies are the result of magnetic inhibition of convection in cool young stars by using magnetic stellar evolution isochrones to determine the age of the Upper Scorpius subgroup of the Scorpius-Centaurus OB Association. A median age of 10 Myr consistent across spectral types A through M is found, except for a subset of F-type stars that appear significantly older. Agreement is shown for ages derived from the Hertzsprung-Russell diagram and from the empirical mass-radius relationship defined by eclipsing multiple-star systems. Surface magnetic field strengths required to produce agreement are of order 2.5 kG and are predicted from a priori estimates of equipartition values. A region in the HR diagram is identified that plausibly connects stars whose structures are weakly influenced by the presence of magnetic fields with those whose structures are strongly influenced by magnetic fields. The models suggest this region is characterized by stars with rapidly thinning outer convective envelopes where the radiative core mass is greater than 75% of the total stellar mass. Furthermore, depletion of lithium predicted from magnetic models appears in better agreement with observed lithium equivalent widths than predictions from non-magnetic models. These results suggest that magnetic inhibition of convection plays an important role in the early evolution of low-mass stars and that it may be responsible for noted age discrepancies in young stellar populations., Comment: 11 pages, 6 figures, 2 tables. Accepted to A&A. Models available online: https://github.com/gfeiden/MagneticUpperSco/
- Published
- 2016
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19. Zodiacal Exoplanets in Time (ZEIT) III: A short-period planet orbiting a pre-main-sequence star in the Upper Scorpius OB Association
- Author
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Aaron C. Rizzuto, David Charbonneau, Andrew Vanderburg, Marshall C. Johnson, Eric Gaidos, Michael J. Ireland, Daniel T. Jaffe, Adam L. Kraus, Gregory A. Feiden, Benjamin Kidder, Megan Ansdell, Jonathan Irwin, Andrew W. Mann, Elisabeth R. Newton, Gregory N. Mace, David James, and Kevin R. Covey
- Subjects
Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Zodiacal light ,010308 nuclear & particles physics ,Astronomy ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Planetary system ,01 natural sciences ,Exoplanet ,Orb (astrology) ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Planet ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,10. No inequality ,010303 astronomy & astrophysics ,Pre-main-sequence star ,Astrophysics::Galaxy Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We confirm and characterize a close-in ($P_{\rm{orb}}$ = 5.425 days), super-Neptune sized ($5.04^{+0.34}_{-0.37}$ Earth radii) planet transiting K2-33 (2MASS J16101473-1919095), a late-type (M3) pre-main sequence (11 Myr-old) star in the Upper Scorpius subgroup of the Scorpius-Centaurus OB association. The host star has the kinematics of a member of the Upper Scorpius OB association, and its spectrum contains lithium absorption, an unambiguous sign of youth (, Accepted to AJ. 17 pages, 10 figures, 3 tables
- Published
- 2016
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20. Parallaxes of metal-poor main-sequence stars
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Ata Sarajedini, Gregory A. Feiden, Barbara McArthur, Edmund P. Nelan, Richard J. Patterson, Andrew McWilliam, Brian Chaboyer, T. E. Harrison, and G. F. Benedict
- Subjects
Physics ,Photometry (astronomy) ,Stars ,Spiral galaxy ,Space and Planetary Science ,K-type main-sequence star ,Stellar collision ,Astronomy ,Astronomy and Astrophysics ,Astrometry ,Astrophysics ,Main sequence ,Blue straggler - Abstract
Our team was awarded 108 orbits of Hubble Space Telescope time to obtain parallaxes and photometry of nine metal-poor stars with [Fe/H] < −1.5 dex. The parallaxes are obtained from observations with the Fine Guidance Sensor (FGS 1r; 11 orbits per star) and photometry was obtained with the Advanced Camera for Surveys (one orbit per star). The first data were obtained in October 2008, and the data collection is ongoing. It is anticipated that the observations will be complete in June 2013. Preliminary data reduction has been completed for five of our target stars. The parallax errors vary from 0.12 to 0.16 milli-arcseconds, and the parallaxes are at least an order of magnitude more accurate than existing Hipparcos parallaxes for these stars. The errors in the true distance modulus range from 0.02 to 0.03 mag. Ground-based high-resolution spectra have been analyzed to obtain accurate abundances for three stars. The properties of the two stars with accurate abundances and parallaxes are in excellent agreement with those predicted by stellar evolution models.
- Published
- 2012
21. Kepler-445, Kepler-446 and the Occurrence of Compact Multiples Orbiting mid-M Dwarf Stars
- Author
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Philip S. Muirhead, Andrew Vanderburg, Timothy D. Morton, Eric Gaidos, Gregory A. Feiden, Adam L. Kraus, Jonathan J. Swift, Andrew W. Mann, Michael J. Ireland, and J. Zachary Gazak
- Subjects
010504 meteorology & atmospheric sciences ,fundamental parameters [stars] ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Protoplanetary disk ,01 natural sciences ,Astronomi, astrofysik och kosmologi ,Planet ,individual (KOI-2704 [stars] ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Astronomy, Astrophysics and Cosmology ,low-mass [stars] ,010303 astronomy & astrophysics ,Stellar density ,planetary systems ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Barnard's Star) ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Kepler-42 ,Astronomy and Astrophysics ,Radius ,Light curve ,KOI-2842 ,Accretion (astrophysics) ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,late-type [stars] ,Astrophysics::Earth and Planetary Astrophysics ,Protoplanet ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We confirm and characterize the exoplanetary systems Kepler-445 and Kepler-446: two mid-M dwarf stars, each with multiple, small, short-period transiting planets. Kepler-445 is a metal-rich ([Fe/H]=+0.25 $\pm$ 0.10) M4 dwarf with three transiting planets, and Kepler-446 is a metal-poor ([Fe/H]=-0.30 $\pm$ 0.10) M4 dwarf also with three transiting planets. Kepler-445c is similar to GJ 1214b: both in planetary radius and the properties of the host star. The Kepler-446 system is similar to the Kepler-42 system: both are metal-poor with large galactic space velocities and three short-period, likely-rocky transiting planets that were initially assigned erroneously large planet-to-star radius ratios. We independently determined stellar parameters from spectroscopy and searched for and fitted the transit light curves for the planets, imposing a strict prior on stellar density in order to remove correlations between the fitted impact parameter and planet-to-star radius ratio for short-duration transits. Combining Kepler-445, Kepler-446 and Kepler-42, and isolating all mid-M dwarf stars observed by Kepler with the precision necessary to detect similar systems, we calculate that 21 $^{+7}_{-5}$ % of mid-M dwarf stars host compact multiples (multiple planets with periods of less than 10 days) for a wide range of metallicities. We suggest that the inferred planet masses for these systems support highly efficient accretion of protoplanetary disk metals by mid-M dwarf protoplanets., Comment: Accepted to The Astrophysical Journal
- Published
- 2015
22. Stellar diameters and temperatures - VI. High angular resolution measurements of the transiting exoplanet host stars HD 189733 and HD 209458 and implications for models of cool dwarfs
- Author
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Stephen R. Kane, Gail H. Schaefer, Gregory A. Feiden, Gerard T. van Belle, Jeremy Jones, Pierre Demarque, Stephen T. Ridgway, Daniel Huber, Laszlo Sturmann, Chris Farrington, David R. Ciardi, Nils H. Turner, Sarbani Basu, Tabetha S. Boyajian, P. J. Goldfinger, T. ten Brummelaar, C. Brooke Lamell, Kaspar von Braun, Mercedes Lopez-Morales, Andrew W. Mann, Vicente Maestro, Debra A. Fischer, John M. Brewer, Harold A. McAlister, Federico Spada, Timothy R. White, and Michael J. Ireland
- Subjects
fundamental parameters [stars] ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,CHARA array ,Astronomi, astrofysik och kosmologi ,Planet ,individual: HD 189733 [stars] ,0103 physical sciences ,Astronomy, Astrophysics and Cosmology ,Spectroscopy ,010303 astronomy & astrophysics ,O-type main-sequence star ,Solar and Stellar Astrophysics (astro-ph.SR) ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,individual: HD 209458 [stars] ,010308 nuclear & particles physics ,stars [infrared] ,Astronomy ,Astronomy and Astrophysics ,Exoplanet ,interferometric [techniques] ,Radial velocity ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Orbital motion ,late-type [stars] ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present direct radii measurements of the well-known transiting exoplanet host stars HD 189733 and HD 209458 using the CHARA Array interferometer. We find the limb-darkened angular diameters to be theta_LD = 0.3848 +/- 0.0055 and 0.2254 +/- 0.0072 milliarcsec for HD 189733 and HD 209458, respectively. HD 189733 and HD 209458 are currently the only two transiting exoplanet systems where detection of the respective planetary companion's orbital motion from high resolution spectroscopy has revealed absolute masses for both star and planet. We use our new measurements together with the orbital information from radial velocity and photometric time series data, Hipparcos distances, and newly measured bolometric fluxes to determine the stellar effective temperatures (T_eff = 4875 +/- 43, 6093 +/- 103 K), stellar linear radii (R_* = 0.805 +/- 0.016, 1.203 +/- 0.061 R_sun), mean stellar densities (rho_* = 1.62 +/- 0.11, 0.58 +/- 0.14 rho_sun), planetary radii (R_p = 1.216 +/- 0.024, 1.451 +/- 0.074 R_Jup), and mean planetary densities (rho_p = 0.605 +/- 0.029, 0.196 +/- 0.033 rho_Jup) for HD 189733 b and HD 209458 b, respectively. The stellar parameters for HD 209458, a F9 dwarf, are consistent with indirect estimates derived from spectroscopic and evolutionary modeling. However, we find that models are unable to reproduce the observational results for the K2 dwarf, HD 189733. We show that, for stellar evolutionary models to match the observed stellar properties of HD 189733, adjustments lowering the solar-calibrated mixing length parameter from 1.83 to 1.34 need to be employed.
- Published
- 2015
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23. Testing Metal-poor Stellar Models and Isochrones withHSTParallaxes of Metal-poor Stars
- Author
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Andrew McWilliam, Barbara McArthur, Thomas E. Harrison, G. F. Benedict, Brian Chaboyer, Edmund P. Nelan, Gregory A. Feiden, Richard J. Patterson, Ata Sarajedini, and Erin M. O'Malley
- Subjects
Physics ,010308 nuclear & particles physics ,Monte Carlo method ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,Photometry (optics) ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Globular cluster ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Color transformation ,Astrophysics::Earth and Planetary Astrophysics ,Parallax ,010303 astronomy & astrophysics ,Stellar evolution ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,Main sequence - Abstract
Hubble Space Telescope (HST) fine guidance sensor observations were used to obtain parallaxes of eight metal-poor ([Fe/H] < -1.4) stars. The parallaxes of these stars determined by the revised Hipparcos reduction average 17% accuracy, in contrast to our new HST parallaxes which average 1% accuracy and have errors on the individual parallaxes ranging from 85 to 144 microarcsecond. This parallax data has been combined with HST ACS photometry in the F606W and F814W filters to obtain the absolute magnitudes of the stars with an accuracy of 0.02 to 0.03 magnitudes. Six of these stars are on the main sequence (with -2.7 < [Fe/H] < -1.8), and suitable for testing metal-poor stellar evolution models and determining the distances to metal-poor globular clusters. Using the abundances obtained by O'Malley et al. (2017) we find that standard stellar models using the Vandenberg & Clem (2003) color transformation do a reasonable job of matching five of the main sequence stars, with HD 54639 ([Fe/H] = -2.5) being anomalous in its location in the color-magnitude diagram. Stellar models and isochrones were generated using a Monte Carlo analysis to take into account uncertainties in the models. Isochrones which fit the parallax stars were used to determine the distances and ages of nine globular clusters (with -2.4, 37 pages, 10 figures
- Published
- 2017
24. Characterizing the Cool KOIs. VI. H- and K-band Spectra of Kepler M Dwarf Planet-candidate Hosts
- Author
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Ellen M. Price, Bárbara Rojas-Ayala, Christoph Baranec, Rachel Thorp, Juliette C. Becker, Reed Riddle, Kevin R. Covey, James P. Lloyd, Andrew Vanderburg, John Asher Johnson, Everett Schlawin, Nicholas M. Law, Gregory A. Feiden, Philip S. Muirhead, and Katherine Hamren
- Subjects
Physics ,Dwarf star ,010504 meteorology & atmospheric sciences ,Dwarf planet ,NASA Exoplanet Archive ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Stellar classification ,01 natural sciences ,Spectral line ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Astronomi, astrofysik och kosmologi ,13. Climate action ,Space and Planetary Science ,Planet ,0103 physical sciences ,Astronomy, Astrophysics and Cosmology ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,0105 earth and related environmental sciences ,Visual binary - Abstract
We present H- and K-band spectra for late-type Kepler Objects of Interest (the "Cool KOIs"): low-mass stars with transiting-planet candidates discovered by NASA's Kepler Mission that are listed on the NASA Exoplanet Archive. We acquired spectra of 103 Cool KOIs and used the indices and calibrations of Rojas-Ayala et al. to determine their spectral types, stellar effective temperatures and metallicities, significantly augmenting previously published values. We interpolate our measured effective temperatures and metallicities onto evolutionary isochrones to determine stellar masses, radii, luminosities and distances, assuming the stars have settled onto the main-sequence. As a choice of isochrones, we use a new suite of Dartmouth predictions that reliably include mid-to-late M dwarf stars. We identify five M4V stars: KOI-961 (confirmed as Kepler 42), KOI-2704, KOI-2842, KOI-4290, and the secondary component to visual binary KOI-1725, which we call KOI-1725 B. We also identify a peculiar star, KOI-3497, which has a Na and Ca lines consistent with a dwarf star but CO lines consistent with a giant. Visible-wavelength adaptive optics imaging reveals two objects within a 1 arc second diameter; however, the objects' colors are peculiar. The spectra and properties presented in this paper serve as a resource for prioritizing follow-up observations and planet validation efforts for the Cool KOIs, and are all available for download online using the "data behind the figure" feature., Comment: Accepted for publication in the Astrophysical Journal Supplement Series (ApJS). Data and table are available in the source
- Published
- 2014
25. Empirical Tests of Pre-Main-Sequence Stellar Evolution Models with Eclipsing Binaries
- Author
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Gregory A. Feiden, Keivan G. Stassun, and Guillermo Torres
- Subjects
Physics ,Sequence ,Diagram ,FOS: Physical sciences ,Astronomy and Astrophysics ,Apparent age ,Astrophysics ,Stars ,Current sample ,Astrophysics - Solar and Stellar Astrophysics ,Astronomi, astrofysik och kosmologi ,Space and Planetary Science ,Astronomy, Astrophysics and Cosmology ,Stellar evolution ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
We examine the performance of standard PMS stellar evolution models against the accurately measured properties of a benchmark sample of 26 PMS stars in 13 EB systems. We provide a definitive compilation of all fundamental properties for the EBs. We also provide a definitive compilation of the various PMS model sets. In the H-R diagram, the masses inferred for the individual stars by the models are accurate to better than 10% above 1 Msun, but below 1 Msun they are discrepant by 50-100%. We find evidence that the failure of the models to match the data is linked to the triples in the EB sample; at least half of the EBs possess tertiary companions. Excluding the triples, the models reproduce the stellar masses to better than ~10% in the H-R diagram, down to 0.5 Msun, below which the current sample is fully contaminated by tertiaries. We consider several mechanisms by which a tertiary might cause changes in the EB properties and thus corrupt the agreement with stellar model predictions. We show that the energies of the tertiary orbits are comparable to that needed to potentially explain the scatter in the EB properties through injection of heat, perhaps involving tidal interaction. It seems from the evidence at hand that this mechanism, however it operates in detail, has more influence on the surface properties of the stars than on their internal structure, as the lithium abundances are broadly in good agreement with model predictions. The EBs that are members of young clusters appear individually coeval to within 20%, but collectively show an apparent age spread of ~50%, suggesting true age spreads in young clusters. However, this apparent spread in the EB ages may also be the result of scatter in the EB properties induced by tertiaries. [Abridged], To appear in New Astronomy Reviews
- Published
- 2014
26. Revised age for CM Draconis and WD 1633+572: Toward a resolution of model-observation radius discrepancies
- Author
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Brian Chaboyer and Gregory A. Feiden
- Subjects
Physics ,Proper motion ,White dwarf ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Thin disk ,Astronomi, astrofysik och kosmologi ,Space and Planetary Science ,Thick disk ,Astronomy, Astrophysics and Cosmology ,Halo ,Low Mass ,Stellar evolution ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
We report an age revision for the low-mass detached eclipsing binary CM Draconis and its common proper motion companion, WD 1633+572. An age of 8.5 $\pm$ 3.5 Gyr is found by combining an age estimate for the lifetime of WD 1633+572 and an estimate from galactic space motions. The revised age is greater than a factor of two older than previous estimates. Our results provide consistency between the white dwarf age and the system's galactic kinematics, which reveal the system is a highly probable member of the galactic thick disk. We find the probability that CM Draconis and WD 1633+572 are members of the thick disk is 8500 times greater than the probability that they are members of the thin disk and 170 times greater than the probability they are halo interlopers. If CM Draconis is a member of the thick disk, it is likely enriched in $\alpha$-elements compared to iron by at least 0.2 dex relative to the Sun. This leads to the possibility that previous studies under-estimate the [Fe/H] value, suggesting the system has a near-solar [Fe/H]. Implications for the long-standing discrepancies between the radii of CM Draconis and predictions from stellar evolution theory are discussed. We conclude that CM Draconis is only inflated by about 2% compared to stellar evolution predictions., Comment: Accepted to A&A, 7 pages, 3 figures, 1 table
- Published
- 2014
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27. Magnetic Inhibition of Convection and the Fundamental Properties of Low-Mass Stars. : II. Fully Convective Main-Sequence Stars
- Author
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Brian Chaboyer and Gregory A. Feiden
- Subjects
Physics ,Convection ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Light curve ,Magnetic field ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Astronomi, astrofysik och kosmologi ,Space and Planetary Science ,Astrophysics::Solar and Stellar Astrophysics ,Astronomy, Astrophysics and Cosmology ,Astrophysics::Earth and Planetary Astrophysics ,Low Mass ,Stellar evolution ,Solar and Stellar Astrophysics (astro-ph.SR) ,Main sequence ,Astrophysics::Galaxy Astrophysics ,Dynamo - Abstract
We examine the hypothesis that magnetic fields are inflating the radii of fully convective main sequence stars in detached eclipsing binaries (DEBs). The magnetic Dartmouth stellar evolution code is used to analyze two systems in particular: Kepler-16 and CM Draconis. Magneto-convection is treated assuming stabilization of convection and also by assuming reductions in convective efficiency due to a turbulent dynamo. We find that magnetic stellar models are unable to reproduce the properties of inflated fully convective main sequence stars, unless strong interior magnetic fields in excess of 10 MG are present. Validation of the magnetic field hypothesis given the current generation of magnetic stellar evolution models therefore depends critically on whether the generation and maintenance of strong interior magnetic fields is physically possible. An examination of this requirement is provided. Additionally, an analysis of previous studies invoking the influence of star spots is presented to assess the suggestion that star spots are inflating stars and biasing light curve analyses toward larger radii. From our analysis, we find that there is not yet sufficient evidence to definitively support the hypothesis that magnetic fields are responsible for the observed inflation among fully convective main sequence stars in DEBs., Comment: Accepted for publication in ApJ, 17 pages, 11 figures, 2 tables
- Published
- 2014
28. The G Plus M Eclipsing Binary V530 Orionis: A Stringent Test of Magnetic Stellar Evolution Models for Low-Mass Stars
- Author
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Jeffrey A. Sabby, Guillermo Torres, J. V. Clausen, Claud H. Sandberg Lacy, Krešimir Pavlovski, H. Bruntt, and Gregory A. Feiden
- Subjects
fundamental parameters [stars] ,FOS: Physical sciences ,Binary number ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,individual (V530 Ori) [stars] ,Spectral line ,photometric [techniques] ,eclipsing [binaries] ,Astrophysics::Solar and Stellar Astrophysics ,Fysik ,stellar evolution ,stellar structure ,binary stars ,low mass stars ,Stellar evolution ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,Eclipse ,Physics ,Astronomy and Astrophysics ,NATURAL SCIENCES. Physics ,Abundance of the chemical elements ,PRIRODNE ZNANOSTI. Fizika ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,evolution [stars] ,Physical Sciences ,Astrophysics::Earth and Planetary Astrophysics ,Low Mass - Abstract
We report extensive photometric and spectroscopic observations of the 6.1-day period, G+M-type detached double-lined eclipsing binary V530 Ori, an important new benchmark system for testing stellar evolution models for low-mass stars. We determine accurate masses and radii for the components with errors of 0.7% and 1.3%, as follows: M(A) = 1.0038 +/- 0.0066 M(sun), M(B) = 0.5955 +/- 0.0022 M(sun), R(A) = 0.980 +/- 0.013 R(sun), and R(B) = 0.5873 +/- 0.0067 R(sun). The effective temperatures are 5890 +/- 100 K (G1V) and 3880 +/- 120 K (M1V), respectively. A detailed chemical analysis probing more than 20 elements in the primary spectrum shows the system to have a slightly subsolar abundance, with [Fe/H] = -0.12 +/- 0.08. A comparison with theory reveals that standard models underpredict the radius and overpredict the temperature of the secondary, as has been found previously for other M dwarfs. On the other hand, models from the Dartmouth series incorporating magnetic fields are able to match the observations of the secondary star at the same age as the primary (3 Gyr) with a surface field strength of 2.1 +/- 0.4 kG when using a rotational dynamo prescription, or 1.3 +/- 0.4 kG with a turbulent dynamo approach, not far from our empirical estimate for this star of 0.83 +/- 0.65 kG. The observations are most consistent with magnetic fields playing only a small role in changing the global properties of the primary. The V530 Ori system thus provides an important demonstration that recent advances in modeling appear to be on the right track to explain the long-standing problem of radius inflation and temperature suppression in low-mass stars., 17 pages in emulateapj format, including figures and tables. To appear in The Astrophysical Journal
- Published
- 2014
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29. The rotation-lithium depletion correlation in theβPictoris association and the LDB age determination
- Author
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B. Monard, R. Petrucci, A. Buccino, S. Messina, Silvano Desidera, Gregory A. Feiden, E. Jofre, M. Millward, P. Kehusmaa, A. C. Lanzafame, Ivan A. Curtis, and Biman J. Medhi
- Subjects
Rotation period ,stars: abundances ,starspot [Stars] ,Ciencias Físicas ,FOS: Physical sciences ,chemistry.chemical_element ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Rotation ,01 natural sciences ,purl.org/becyt/ford/1 [https] ,stars: rotation ,stars: activity ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Beta Pictoris ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,Physics ,010308 nuclear & particles physics ,stars: late-type ,Astronomy and Astrophysics ,purl.org/becyt/ford/1.3 [https] ,individual: beta Pictoris association [Stars] ,rotation [Stars] ,Astronomía ,starspots ,stars: individual: betaPictoris association ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,chemistry ,Space and Planetary Science ,late-type [Stars] ,abundances [Stars] ,Lithium ,Astrophysics::Earth and Planetary Astrophysics ,Low Mass ,Pleiades ,Equivalent width ,activity [Stars] ,CIENCIAS NATURALES Y EXACTAS - Abstract
There is evidence in the 125-Myr Pleiades cluster, and more recently in the 5-Myr NGC 2264 cluster, that rotation plays a key role in the Lithium (Li) depletion processes among low-mass stars. Fast rotators appear to be less Li-depleted than equal-mass slow rotators. We intend to explore the existence of a Li depletion - rotation connection among the beta Pictoris members at an age of about 24 Myr, and to use such correlation either to confirm or to improve the age estimate based on the Lithium Depletion Boundary (LDB) modeling. We have photometrically monitored all the known members of the beta Pictoris association with at least one Lithium equivalent width (Li EW) measurement from the literature. We measured the rotation periods of 30 members for the first time and retrieved from the literature the rotation periods for other 36 members, building a catalogue of 66 members with measured rotation period and Li EW. We find that in the 0.3 < M < 0.8 Msun range, there is a strong correlation between rotation and Li EW. For higher mass stars, no significant correlation is found. For very low mass stars in the Li depletion onset, at about 0.1 Msun, data are too few to infer a significant correlation. The observed Li EWs are compared with those predicted by the Dartmouth stellar evolutionary models that incorporate the effects of magnetic fields. After decorrelating the Li EW from the rotation period, we find that the hot side of the LDB is fitted well by Li EW values corresponding to an age of 25$\pm$3 Myr in good agreement with independent estimates from the literature., 8 pages, 6 figures, 1 table, accepted by A&A
- Published
- 2016
30. Magnetic Inhibition of Convection and the Fundamental Properties of Low-Mass Stars. I. Stars with a Radiative Core
- Author
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Gregory A. Feiden and Brian Chaboyer
- Subjects
Physics ,Convection ,Convective heat transfer ,010308 nuclear & particles physics ,Metallicity ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,01 natural sciences ,Magnetic field ,Stars ,Astronomi, astrofysik och kosmologi ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,0103 physical sciences ,Convective mixing ,Radiative transfer ,Astronomy, Astrophysics and Cosmology ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Stellar evolution ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
Magnetic fields are hypothesized to inflate the radii of low-mass stars---defined as less massive than 0.8$M_\odot$---in detached eclipsing binaries (DEBs). We investigate this hypothesis using the recently introduced magnetic Dartmouth stellar evolution code. In particular, we focus on stars thought to have a radiative core and convective outer envelope by studying in detail three individual DEBs: UV Psc, YY Gem, and CU Cnc. The results suggest that the stabilization of thermal convection by a magnetic field is a plausible explanation for the observed model-radius discrepancies. However, surface magnetic field strengths required by the models are significantly stronger than those estimated from the observed coronal X-ray emission. Agreement between model predicted surface magnetic field strengths and those inferred from X-ray observations can be found by assuming that the magnetic field sources its energy from convection. This approach makes the transport of heat by convection less efficient and is akin to reduced convective mixing length methods used in other studies. Predictions for the metallicity and magnetic field strengths of the aforementioned systems are reported. We also develop an expression relating a reduction in the convective mixing length to a magnetic field strength in units of the equipartition value. Our results are compared with those from previous investigations to incorporate magnetic fields to explain the low-mass DEB radius inflation. Finally, we explore how the effects of magnetic fields might affect mass determinations using asteroseismic data and the implication of magnetic fields on exoplanet studies., Accepted for publication in ApJ, 25 pages, 19 figures, 6 tables. Version 2 is the final manuscript
- Published
- 2013
31. The Interior Structure Constants as an Age Diagnostic for Low-Mass, Pre-Main Sequence Detached Eclipsing Binary Stars
- Author
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Aaron Dotter and Gregory A. Feiden
- Subjects
Physics ,010308 nuclear & particles physics ,Apsidal precession ,FOS: Physical sciences ,Astronomy and Astrophysics ,Orbital eccentricity ,Astrophysics ,01 natural sciences ,Astrophysics - Astrophysics of Galaxies ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,Binary star ,Astrophysics::Solar and Stellar Astrophysics ,Stellar structure ,Astrophysics::Earth and Planetary Astrophysics ,Low Mass ,010303 astronomy & astrophysics ,Stellar evolution ,Main sequence ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
We propose a novel method for determining the ages of low-mass, pre-main sequence stellar systems using the apsidal motion of low-mass detached eclipsing binaries. The apsidal motion of a binary system with an eccentric orbit provides information regarding the interior structure constants of the individual stars. These constants are related to the normalized stellar interior density distribution and can be extracted from the predictions of stellar evolution models. We demonstrate that low-mass, pre-main sequence stars undergoing radiative core contraction display rapidly changing interior structure constants (greater than 5% per 10 Myr) that, when combined with observational determinations of the interior structure constants (with 5 -- 10% precision), allow for a robust age estimate. This age estimate, unlike those based on surface quantities, is largely insensitive to the surface layer where effects of magnetic activity are likely to be most pronounced. On the main sequence, where age sensitivity is minimal, the interior structure constants provide a valuable test of the physics used in stellar structure models of low-mass stars. There are currently no known systems where this technique is applicable. Nevertheless, the emphasis on time domain astronomy with current missions, such as Kepler, and future missions, such as LSST, has the potential to discover systems where the proposed method will be observationally feasible., Accepted for publication in ApJ, 8 pages, 3 figures
- Published
- 2013
32. Do Magnetic Fields Actually Inflate Low-Mass Stars?
- Author
-
Brian Chaboyer and Gregory A. Feiden
- Subjects
Physics ,Convection ,Convective heat transfer ,Metallicity ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Magnetic flux ,Magnetic field ,Luminosity ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Stellar evolution ,Astrophysics::Galaxy Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
Magnetic fields have been hypothesized to inflate the radii of low-mass stars---defined as less than 0.8 solar masses---in detached eclipsing binaries (DEBs). We evaluate this hypothesis using the magnetic Dartmouth stellar evolution code. Results suggest that magnetic suppression of thermal convection can inflate low-mass stars that possess a radiative core and convective outer envelope. A scaling relation between X-ray luminosity and surface magnetic flux indicates that model surface magnetic field strength predictions are consistent with observations. This supports the notion that magnetic fields may be inflating these stars. However, magnetic models are unable to reproduce radii of fully convective stars in DEBs. Instead, we propose that model discrepancies below the fully convective boundary are related to metallicity., Comment: 4 pages, 3 figures, to appear in proceedings from IAU Symp. 302: "Magnetic Fields Throughout Stellar Evolution"
- Published
- 2013
- Full Text
- View/download PDF
33. ERRATUM: 'HOW TO CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, AND RADIUS' (ApJ, 804, 64)
- Author
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Kaspar von Braun, Tabetha S. Boyajian, Gregory A. Feiden, Eric Gaidos, and Andrew W. Mann
- Subjects
Physics ,010308 nuclear & particles physics ,Bolometer ,Astronomy ,Astronomy and Astrophysics ,Astrophysics ,Radius ,Effective temperature ,01 natural sciences ,law.invention ,Luminosity ,Space and Planetary Science ,law ,0103 physical sciences ,010303 astronomy & astrophysics - Published
- 2016
34. Age and helium content of the open cluster NGC 6791 from multiple eclipsing binary members. II. age dependencies and new insights
- Author
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Eric L. Sandquist, Luigi R. Bedin, Karsten Brogaard, Antonino Milone, Dennis Stello, Jens Jessen-Hansen, Hans Bruntt, Peter B. Stetson, Frank Grundahl, Aaron Dotter, Gregory A. Feiden, S. Frandsen, Andrea Miglio, and Don A. VandenBerg
- Subjects
Physics ,Binary number ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Asteroseismology ,Blue straggler ,Photometry (optics) ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Binary star ,Astrophysics::Solar and Stellar Astrophysics ,Stellar structure ,Astrophysics::Earth and Planetary Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,Open cluster - Abstract
Models of stellar structure and evolution can be constrained by measuring accurate parameters of detached eclipsing binaries in open clusters. Multiple binary stars provide the means to determine helium abundances in these old stellar systems, and in turn, to improve estimates of their age. In the first paper of this series, we demonstrated how measurements of multiple eclipsing binaries in the old open cluster NGC6791 sets tighter constraints on the properties of stellar models than has previously been possible, thereby potentially improving both the accuracy and precision of the cluster age. Here we add additional constraints and perform an extensive model comparison to determine the best estimates of the cluster age and helium content, employing as many observational constraints as possible. We improve our photometry and correct empirically for differential reddening effects. We then perform an extensive comparison of the CMDs and eclipsing binary measurements to Victoria and DSEP isochrones to estimate cluster parameters. We also reanalyse a spectrum of the star 2-17 to improve [Fe/H] constraints. We find a best estimate of the age of ~8.3 Gyr while demonstrating that remaining age uncertainty is dominated by uncertainties in the CNO abundances. The helium mass fraction is well constrained at Y = 0.30 \pm 0.01 resulting in dY/dZ ~ 1.4 assuming that such a relation exists. During the analysis we firmly identify blue straggler stars, including the star 2-17, and find indications for the presence of their evolved counterparts. Our analysis supports the RGB mass-loss found from asteroseismology and we determine precisely the absolute mass of stars on the lower RGB, 1.15\pm0.02Msun. This will be an important consistency check for the detailed asteroseismology of cluster stars., 18 Pages, 9 Figures, accepted for publication in A&A
- Published
- 2012
35. Self-Consistent Magnetic Stellar Evolution Models of the Detached, Solar-Type Eclipsing Binary EF Aquarii
- Author
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Gregory A. Feiden and Brian Chaboyer
- Subjects
Physics ,Model photosphere ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Effective temperature ,01 natural sciences ,7. Clean energy ,K-line ,Magnetic field ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,0103 physical sciences ,ROSAT ,Astrophysics::Solar and Stellar Astrophysics ,Stellar structure ,Astrophysics::Earth and Planetary Astrophysics ,010306 general physics ,010303 astronomy & astrophysics ,Stellar evolution ,Astrophysics::Galaxy Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
We introduce a new one-dimensional stellar evolution code, based on the existing Dartmouth code, that self-consistently accounts for the presence of a globally pervasive magnetic field. The methods involved in perturbing the equations of stellar structure, the equation of state, and the mixing-length theory of convection are presented and discussed. As a first test of the code's viability, stellar evolution models are computed for the components of a solar-type, detached eclipsing binary (DEB) system, EF Aquarii, shown to exhibit large disagreements with stellar models. The addition of the magnetic perturbation corrects the radius and effective temperature discrepancies observed in EF Aquarii. Furthermore, the required magnetic field strength at the model photosphere is within a factor of two of the magnetic field strengths estimated from the stellar X-ray luminosities measured by ROSAT and those predicted from Ca II K line core emission. These models provide firm evidence that the suppression of thermal convection arising from the presence of a magnetic field is sufficient to significantly alter the structure of solar-type stars, producing noticeably inflated radii and cooler effective temperatures. The inclusion of magnetic effects within a stellar evolution model has a wide range of applications, from DEBs and exoplanet host stars to the donor stars of cataclysmic variables., Comment: Accepted for publication in ApJ, 15 pages, 3 figures; Misprints are corrected in version 2
- Published
- 2012
- Full Text
- View/download PDF
36. Reevaluating the Mass-Radius Relation for Low-Mass, Main Sequence Stars
- Author
-
Brian Chaboyer and Gregory A. Feiden
- Subjects
Physics ,education.field_of_study ,010504 meteorology & atmospheric sciences ,Metallicity ,Population ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Radius ,01 natural sciences ,Galaxy ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,0103 physical sciences ,Binary star ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,education ,010303 astronomy & astrophysics ,Stellar evolution ,Astrophysics::Galaxy Astrophysics ,Main sequence ,Solar and Stellar Astrophysics (astro-ph.SR) ,0105 earth and related environmental sciences - Abstract
We examine the agreement between the observed and theoretical low-mass (< 0.8 solar masses) stellar main sequence mass-radius relationship by comparing detached eclipsing binary (DEB) data with a new, large grid of stellar evolution models. The new grid allows for a realistic variation in the age and metallicity of the DEB population, characteristic of the local galactic neighborhood. Overall, our models do a reasonable job of reproducing the observational data. A large majority of the models match the observed stellar radii to within 4%, with a mean absolute error of 2.3%. These results represent a factor of two improvement compared to previous examinations of the low-mass mass-radius relationship. The improved agreement between models and observations brings the radius deviations within the limits imposed by potential starspot-related uncertainties for 92% of the stars in our DEB sample., 16 pages, 5 figures, Accepted for publication in ApJ
- Published
- 2012
- Full Text
- View/download PDF
37. Accurate Low-Mass Stellar Models of KOI-126
- Author
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Brian Chaboyer, Gregory A. Feiden, and Aaron Dotter
- Subjects
Physics ,Convection ,Equation of state ,010504 meteorology & atmospheric sciences ,Apsidal precession ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Stars ,Orbit ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Dispersion (water waves) ,Low Mass ,010303 astronomy & astrophysics ,Stellar evolution ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences - Abstract
The recent discovery of an eclipsing hierarchical triple system with two low-mass stars in a close orbit (KOI-126) by Carter et al. (2011) appeared to reinforce the evidence that theoretical stellar evolution models are not able to reproduce the observational mass-radius relation for low-mass stars. We present a set of stellar models for the three stars in the KOI-126 system that show excellent agreement with the observed radii. This agreement appears to be due to the equation of state implemented by our code. A significant dispersion in the observed mass-radius relation for fully convective stars is demonstrated; indicative of the influence of physics currently not incorporated in standard stellar evolution models. We also predict apsidal motion constants for the two M-dwarf companions. These values should be observationally determined to within 1% by the end of the Kepler mission., 5 pages, 2 figures, Accepted for publication to ApJL
- Published
- 2011
38. HOW TO CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, AND RADIUS
- Author
-
Gregory A. Feiden, Eric Gaidos, Andrew W. Mann, Kaspar von Braun, and Tabetha S. Boyajian
- Subjects
Absolute magnitude ,Metallicity ,fundamental parameters [stars] ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Spectral line ,Luminosity ,Astronomi, astrofysik och kosmologi ,Astrophysics::Solar and Stellar Astrophysics ,Astronomy, Astrophysics and Cosmology ,low-mass [stars] ,planetary systems ,Stellar evolution ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,Physics ,Astronomy and Astrophysics ,Radius ,Effective temperature ,abundances [stars] ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,late-type [stars] ,Astrophysics::Earth and Planetary Astrophysics ,statistics [stars] - Abstract
Precise and accurate parameters for late-type (late K and M) dwarf stars are important for characterization of any orbiting planets, but such determinations have been hampered by these stars' complex spectra and dissimilarity to the Sun. We exploit an empirically calibrated method to estimate spectroscopic effective temperature ($T_{\rm{eff}}$) and the Stefan-Boltzmann law to determine radii of 183 nearby K7-M7 single stars with a precision of 2-5%. Our improved stellar parameters enable us to develop model-independent relations between $T_{\rm{eff}}$ or absolute magnitude and radius, as well as between color and $T_{\rm{eff}}$. The derived $T_{\rm{eff}}$-radius relation depends strongly on [Fe/H], as predicted by theory. The relation between absolute $K_S$ magnitude and radius can predict radii accurate to $\simeq$3%. We derive bolometric corrections to the $VR_CI_CgrizJHK_S$ and Gaia passbands as a function of color, accurate to 1-3%. We confront the reliability of predictions from Dartmouth stellar evolution models using a Markov Chain Monte Carlo to find the values of unobservable model parameters (mass, age) that best reproduce the observed effective temperature and bolometric flux while satisfying constraints on distance and metallicity as Bayesian priors. With the inferred masses we derive a semi-empirical mass-absolute magnitude relation with a scatter of 2% in mass. The best-agreement models over-predict stellar $T_{\rm{eff}}$s by an average of 2.2% and under-predict stellar radii by 4.6%, similar to differences with values from low-mass eclipsing binaries. These differences are not correlated with metallicity, mass, or indicators of activity, suggesting issues with the underlying model assumptions e.g., opacities or convective mixing length., 36 pages, 23 figures, 7 tables. ApJ in press. Machine readable version of Tables 5-7 included with ancillary data
- Published
- 2015
39. BANYAN. IV. FUNDAMENTAL PARAMETERS OF LOW-MASS STAR CANDIDATES IN NEARBY YOUNG STELLAR KINEMATIC GROUPS—ISOCHRONAL AGE DETERMINATION USING MAGNETIC EVOLUTIONARY MODELS
- Author
-
Étienne Artigau, Jonathan Gagné, Loic Albert, René Doyon, Adric R. Riedel, Gregory A. Feiden, David Lafrenière, and Lison Malo
- Subjects
Physics ,Proper motion ,Field (physics) ,Metallicity ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Magnetic field ,Radial velocity ,Stars ,Astronomi, astrofysik och kosmologi ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astronomy, Astrophysics and Cosmology ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,10. No inequality ,Low Mass ,Parallax ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics - Abstract
Based on high resolution optical spectra obtained with ESPaDOnS at CFHT, we determine fundamental parameters (\Teff, R, \Lbol, \logg\ and metallicity) for 59 candidate members of nearby young kinematic groups. The candidates were identified through the BANYAN Bayesian inference method of \citet{2013malo}, which takes into account the position, proper motion, magnitude, color, radial velocity and parallax (when available) to establish a membership probability. The derived parameters are compared to Dartmouth Magnetic evolutionary models and to field stars with the goal to constrain the age of our candidates. We find that, in general, low-mass stars in our sample are more luminous and have inflated radii compared to older stars, a trend expected for pre-main sequence stars. The Dartmouth Magnetic evolutionary models show a good fit to observations of field K and M stars assuming a magnetic field strength of a few kG, as typically observed for cool stars. Using the low-mass members of $\beta$Pictoris moving group, we have re-examined the age inconsistency problem between Lithium Depletion age and isochronal age (Hertzspring-Russell diagram). We find that the inclusion of the magnetic field in evolutionary models increase the isochronal age estimates for the K5V-M5V stars. Using these models and field strengths, we derive an average isochronal age between 15 and 28 Myr and we confirm a clear Lithium Depletion Boundary from which an age of 26$\pm$3~Myr is derived, consistent with previous age estimates based on this method., Comment: Accepted for publication in ApJ
- Published
- 2014
40. Masses and Implications for Ages of Low-mass Pre-main-sequence Stars in Taurus and Ophiuchus.
- Author
-
M. Simon, S. Guilloteau, Tracy L. Beck, E. Chapillon, E. Di Folco, A. Dutrey, Gregory A. Feiden, N. Grosso, V. Piétu, L. Prato, and Gail H. Schaefer
- Subjects
GAS giants ,STELLAR mass ,MAGNETIC fields ,HR diagrams ,STARS ,STELLAR magnetic fields ,AGE of stars - Abstract
The accuracy of masses of pre-main-sequence stars derived from their locations on the Hertzsprung–Russell diagram (HRD) can be tested by comparison with accurate and precise masses determined independently. We present 29 single stars in the Taurus star-forming region (SFR) and 3 in the Ophiuchus SFR with masses measured dynamically to a precision of at least 10%. Our results include 9 updated mass determinations and 3 that have not had their dynamical masses published before. This list of stars with fundamental, dynamical masses, M
dyn , is drawn from a larger list of 39 targets in the Taurus SFR and 6 in the Ophiuchus SFR. Placing the stars with accurate and precise dynamical masses on HRDs that do not include internal magnetic fields underestimates the mass compared to Mdyn by about 30%. Placing them on an HRD that does include magnetic fields yields mass estimates in much better agreement with Mdyn , with an average difference between Mdyn and the estimated track mass of 0.01 ± 0.02 M⊙ . The ages of the stars, 3–10 MY on tracks that include magnetic fields, is older than the 1–3 MY indicated by the nonmagnetic models. The older ages of T Tauri stars predicted by the magnetic models increase the time available for evolution of their disks and formation of the giant gas exoplanets. The agreement between our Mdyn values and the masses on the magnetic field tracks provides indirect support for these older ages. [ABSTRACT FROM AUTHOR]- Published
- 2019
- Full Text
- View/download PDF
41. The Factory and the Beehive. III. PTFEB132.707+19.810, A Low-mass Eclipsing Binary in Praesepe Observed by PTF and K2.
- Author
-
Adam L. Kraus, Stephanie T. Douglas, Andrew W. Mann, Marcel A. Agüeros, Nicholas M. Law, Kevin R. Covey, Gregory A. Feiden, Aaron C. Rizzuto, Andrew W. Howard, Howard Isaacson, Eric Gaidos, Guillermo Torres, and Gaspar Bakos
- Subjects
BINARY stars ,STAR formation ,GALACTIC evolution ,LOW mass stars ,STARSPOTS - Abstract
Theoretical models of stars constitute the fundamental bedrock upon which much of astrophysics is built, but large swaths of model parameter space remain uncalibrated by observations. The best calibrators are eclipsing binaries in clusters, allowing measurement of masses, radii, luminosities, and temperatures for stars of known metallicity and age. We present the discovery and detailed characterization of PTFEB132.707+19.810, a P = 6.0 day eclipsing binary in the Praesepe cluster (τ ∼ 600–800 Myr; [Fe/H] = 0.14 ± 0.04). The system contains two late-type stars (SpT
P = M3.5 ± 0.2; SpTS = M4.3 ± 0.7) with precise masses ( M⊙ ; M⊙ ) and radii ( R⊙ ; R⊙ ). Neither star meets the predictions of stellar evolutionary models. The primary has the expected radius but is cooler and less luminous, while the secondary has the expected luminosity but is cooler and substantially larger (by 20%). The system is not tidally locked or circularized. Exploiting a fortuitous 4:5 commensurability between Porb and , we demonstrate that fitting errors from the unknown spot configuration only change the inferred radii by ≲1%–2%. We also analyze subsets of data to test the robustness of radius measurements; the radius sum is more robust to systematic errors and preferable for model comparisons. We also test plausible changes in limb darkening and find corresponding uncertainties of ∼1%. Finally, we validate our pipeline using extant data for GU Boo, finding that our independent results match previous radii to within the mutual uncertainties (2%–3%). We therefore suggest that the substantial discrepancies are astrophysical; since they are larger than those for old field stars, they may be tied to the intermediate age of PTFEB132.707+19.810. [ABSTRACT FROM AUTHOR]- Published
- 2017
- Full Text
- View/download PDF
42. ZODIACAL EXOPLANETS IN TIME (ZEIT). III. A SHORT-PERIOD PLANET ORBITING A PRE-MAIN-SEQUENCE STAR IN THE UPPER SCORPIUS OB ASSOCIATION.
- Author
-
Andrew W. Mann, Elisabeth R. Newton, Aaron C. Rizzuto, Jonathan Irwin, Gregory A. Feiden, Eric Gaidos, Gregory N. Mace, Adam L. Kraus, David J. James, Megan Ansdell, David Charbonneau, Kevin R. Covey, Michael J. Ireland, Daniel T. Jaffe, Marshall C. Johnson, Benjamin Kidder, and Andrew Vanderburg
- Published
- 2016
- Full Text
- View/download PDF
43. ERRATUM: “HOW TO CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, AND RADIUS” (ApJ, 804, 64).
- Author
-
Andrew W. Mann, Gregory A. Feiden, Eric Gaidos, Tabetha Boyajian, and Kaspar von Braun
- Subjects
- *
DWARF stars , *STELLAR luminosity function - Abstract
A correction to the article "How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass and Radius" is presented.
- Published
- 2016
- Full Text
- View/download PDF
44. HOW TO CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, AND RADIUS.
- Author
-
Andrew W. Mann, Gregory A. Feiden, Eric Gaidos, Tabetha Boyajian, and Kaspar von Braun
- Subjects
- *
DWARF stars , *STELLAR populations , *CLASSIFICATION of stars , *LOW mass stars , *PLANETARY orbits - Abstract
Precise and accurate parameters for late-type (late K and M) dwarf stars are important for characterization of any orbiting planets, but such determinations have been hampered by these stars’ complex spectra and dissimilarity to the Sun. We exploit an empirically calibrated method to estimate spectroscopic effective temperature (Teff) and the Stefan–Boltzmann law to determine radii of 183 nearby K7–M7 single stars with a precision of 2%–5%. Our improved stellar parameters enable us to develop model-independent relations between Teff or absolute magnitude and radius, as well as between color and Teff. The derived Teff–radius relation depends strongly on [Fe/H], as predicted by theory. The relation between absolute KS magnitude and radius can predict radii accurate to 3%. We derive bolometric corrections to the and Gaia passbands as a function of color, accurate to 1%–3%. We confront the reliability of predictions from Dartmouth stellar evolution models using a Markov chain Monte Carlo to find the values of unobservable model parameters (mass, age) that best reproduce the observed effective temperature and bolometric flux while satisfying constraints on distance and metallicity as Bayesian priors. With the inferred masses we derive a semi-empirical mass–absolute magnitude relation with a scatter of 2% in mass. The best-agreement models overpredict stellar Teff values by an average of 2.2% and underpredict stellar radii by 4.6%, similar to differences with values from low-mass eclipsing binaries. These differences are not correlated with metallicity, mass, or indicators of activity, suggesting issues with the underlying model assumptions, e.g., opacities or convective mixing length. [ABSTRACT FROM AUTHOR]
- Published
- 2015
- Full Text
- View/download PDF
45. Wind models for M-type AGB stars in LMC
- Author
-
Bladh, Sara and Gregory A. Feiden
- Subjects
cool stars 19 ,AGB/Supergiant splinter session - Abstract
The power-presentation from my talk "Wind models for M-type AGB stars in LMC"
- Published
- 2016
- Full Text
- View/download PDF
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