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51. Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields

Author

Keegans, James D., primary, Pignatari, Marco, additional, Stancliffe, Richard J., additional, Travaglio, Claudia, additional, Jones, Samuel, additional, Gibson, Brad K., additional, Townsley, Dean M., additional, Miles, Broxton J., additional, Shen, Ken J., additional, and Few, Gareth, additional

Published
2023
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52. The chemical evolution of the solar neighbourhood for planet-hosting stars

Author

Pignatari, Marco, primary, Trueman, Thomas C L, additional, Womack, Kate A, additional, Gibson, Brad K, additional, Côté, Benoit, additional, Turrini, Diego, additional, Sneden, Christopher, additional, Mojzsis, Stephen J, additional, Stancliffe, Richard J, additional, Fong, Paul, additional, Lawson, Thomas V, additional, Keegans, James D, additional, Pilkington, Kate, additional, Passy, Jean-Claude, additional, Beers, Timothy C, additional, and Lugaro, Maria, additional

Published
2023
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58. Project ThaiPASS: international outreach blending astronomy and Python

Author

Keegans, James D, primary, Stancliffe, Richard J, additional, Bilton, Lawrence E, additional, Cashmore, Claire R, additional, Gibson, Brad K, additional, Kristensen, Mikkel Theiss, additional, Lawson, Thomas V, additional, Pignatari, Marco, additional, Vaezzadeh, Iraj, additional, Côté, Benoit, additional, and Chongchitnan, Siri, additional

Published
2021
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60. Radioactive nuclei in the early Solar system: analysis of the 15 isotopes produced by core-collapse supernovae.

Author

Lawson, Thomas V, Pignatari, Marco, Stancliffe, Richard J, den Hartogh, Jacqueline, Jones, Sam, Fryer, Chris L, Gibson, Brad K, and Lugaro, Maria

Subjects
SOLAR system, ISOTOPIC analysis, RADIOISOTOPES, SUPERNOVAE, NUCLEAR reactions, TRACE elements
Abstract

Short-lived radioactive isotopes (SLRs) with half-lives between 0.1 and 100 Myr can be used to probe the origin of the Solar system. In this work, we examine the core-collapse supernovae production of the 15 SLRs produced: 26Al, 36Cl, 41Ca, 53Mn, 60Fe, 92Nb, 97Tc, 98Tc, 107Pd, 126Sn, 129I, 135Cs, 146Sm, 182Hf, and 205Pb. We probe the impact of the uncertainties of the core-collapse explosion mechanism by examining a collection of 62 core-collapse models with initial masses of 15, 20, and 25 M⊙, explosion energies between 3.4 × 1050 and 1.8 × 1052 erg and compact remnant masses between 1.5 and 4.89 M⊙. We identify the impact of both explosion energy and remnant mass on the final yields of the SLRs. Isotopes produced within the innermost regions of the star, such as 92Nb and 97Tc, are the most affected by the remnant mass, 92Nb varying by five orders of magnitude. Isotopes synthesized primarily in explosive C-burning and explosive He-burning, such as 60Fe, are most affected by explosion energies. 60Fe increases by two orders of magnitude from the lowest to the highest explosion energy in the 15 M⊙ model. The final yield of each examined SLR is used to compare to literature models. [ABSTRACT FROM AUTHOR]

Published
2022
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63. Molecular evolutionary trends and feeding ecology diversification in the Hemiptera, anchored by the milkweed bug genome

Author

Panfilio, Kristen A., Vargas Jentzsch, Iris M., Benoit, Joshua B., Erezyilmaz, Deniz, Suzuki, Yuichiro, Colella, Stefano, Robertson, Hugh M., Poelchau, Monica F., Waterhouse, Robert M., Ioannidis, Panagiotis, Weirauch, Matthew T., Hughes, Daniel S. T., Murali, Shwetha C., Werren, John H., Jacobs, Chris G. C., Duncan, Elizabeth J., Armisén, David, Vreede, Barbara M. I., Baa-Puyoulet, Patrice, Berger, Chloé S., Chang, Chun-che, Chao, Hsu, Chen, Mei-Ju M., Chen, Yen-Ta, Childers, Christopher P., Chipman, Ariel D., Cridge, Andrew G., Crumière, Antonin J. J., Dearden, Peter K., Didion, Elise M., Dinh, Huyen, Doddapaneni, Harsha Vardhan, Dolan, Amanda, Dugan, Shannon, Extavour, Cassandra G., Febvay, Gérard, Friedrich, Markus, Ginzburg, Neta, Han, Yi, Heger, Peter, Holmes, Christopher J., Horn, Thorsten, Hsiao, Yi-min, Jennings, Emily C., Johnston, J. Spencer, Jones, Tamsin E., Jones, Jeffery W., Khila, Abderrahman, Koelzer, Stefan, Kovacova, Viera, Leask, Megan, Lee, Sandra L., Lee, Chien-Yueh, Lovegrove, Mackenzie R., Lu, Hsiao-ling, Lu, Yong, Moore, Patricia J., Munoz-Torres, Monica C., Muzny, Donna M., Palli, Subba R., Parisot, Nicolas, Pick, Leslie, Porter, Megan L., Qu, Jiaxin, Refki, Peter N., Richter, Rose, Rivera-Pomar, Rolando, Rosendale, Andrew J., Roth, Siegfried, Sachs, Lena, Santos, M. Emília, Seibert, Jan, Sghaier, Essia, Shukla, Jayendra N., Stancliffe, Richard J., Tidswell, Olivia, Traverso, Lucila, van der Zee, Maurijn, Viala, Séverine, Worley, Kim C., Zdobnov, Evgeny M., Gibbs, Richard A., Richards, Stephen, Panfilio, Kristen A., Vargas Jentzsch, Iris M., Benoit, Joshua B., Erezyilmaz, Deniz, Suzuki, Yuichiro, Colella, Stefano, Robertson, Hugh M., Poelchau, Monica F., Waterhouse, Robert M., Ioannidis, Panagiotis, Weirauch, Matthew T., Hughes, Daniel S. T., Murali, Shwetha C., Werren, John H., Jacobs, Chris G. C., Duncan, Elizabeth J., Armisén, David, Vreede, Barbara M. I., Baa-Puyoulet, Patrice, Berger, Chloé S., Chang, Chun-che, Chao, Hsu, Chen, Mei-Ju M., Chen, Yen-Ta, Childers, Christopher P., Chipman, Ariel D., Cridge, Andrew G., Crumière, Antonin J. J., Dearden, Peter K., Didion, Elise M., Dinh, Huyen, Doddapaneni, Harsha Vardhan, Dolan, Amanda, Dugan, Shannon, Extavour, Cassandra G., Febvay, Gérard, Friedrich, Markus, Ginzburg, Neta, Han, Yi, Heger, Peter, Holmes, Christopher J., Horn, Thorsten, Hsiao, Yi-min, Jennings, Emily C., Johnston, J. Spencer, Jones, Tamsin E., Jones, Jeffery W., Khila, Abderrahman, Koelzer, Stefan, Kovacova, Viera, Leask, Megan, Lee, Sandra L., Lee, Chien-Yueh, Lovegrove, Mackenzie R., Lu, Hsiao-ling, Lu, Yong, Moore, Patricia J., Munoz-Torres, Monica C., Muzny, Donna M., Palli, Subba R., Parisot, Nicolas, Pick, Leslie, Porter, Megan L., Qu, Jiaxin, Refki, Peter N., Richter, Rose, Rivera-Pomar, Rolando, Rosendale, Andrew J., Roth, Siegfried, Sachs, Lena, Santos, M. Emília, Seibert, Jan, Sghaier, Essia, Shukla, Jayendra N., Stancliffe, Richard J., Tidswell, Olivia, Traverso, Lucila, van der Zee, Maurijn, Viala, Séverine, Worley, Kim C., Zdobnov, Evgeny M., Gibbs, Richard A., and Richards, Stephen

Published
2019

68. Molecular evolutionary trends and feeding ecology diversification in the Hemiptera, anchored by the milkweed bug genome

Author

Panfilio, Kristen A., primary, Jentzsch, Iris M. Vargas, additional, Benoit, Joshua B., additional, Erezyilmaz, Deniz, additional, Suzuki, Yuichiro, additional, Colella, Stefano, additional, Robertson, Hugh M., additional, Poelchau, Monica F., additional, Waterhouse, Robert M., additional, Ioannidis, Panagiotis, additional, Weirauch, Matthew T., additional, Hughes, Daniel S.T., additional, Murali, Shwetha C., additional, Werren, John H., additional, Jacobs, Chris G.C., additional, Duncan, Elizabeth J., additional, Armisén, David, additional, Vreede, Barbara M.I., additional, Baa-Puyoulet, Patrice, additional, Berger, Chloé S., additional, Chang, Chun-che, additional, Chao, Hsu, additional, Chen, Mei-Ju M., additional, Chen, Yen-Ta, additional, Childers, Christopher P., additional, Chipman, Ariel D., additional, Cridge, Andrew G., additional, Crumière, Antonin J.J., additional, Dearden, Peter K., additional, Didion, Elise M., additional, Dinh, Huyen, additional, Doddapaneni, HarshaVardhan, additional, Dolan, Amanda, additional, Dugan, Shannon, additional, Extavour, Cassandra G., additional, Febvay, Gérard, additional, Friedrich, Markus, additional, Ginzburg, Neta, additional, Han, Yi, additional, Heger, Peter, additional, Holmes, Christopher J., additional, Horn, Thorsten, additional, Hsiao, Yi-min, additional, Jennings, Emily C., additional, Johnston, J. Spencer, additional, Jones, Tamsin E., additional, Jones, Jeffery W., additional, Khila, Abderrahman, additional, Koelzer, Stefan, additional, Kovacova, Viera, additional, Leask, Megan, additional, Lee, Sandra L., additional, Lee, Chien-Yueh, additional, Lovegrove, Mackenzie R., additional, Lu, Hsiao-ling, additional, Lu, Yong, additional, Moore, Patricia J., additional, Munoz-Torres, Monica C., additional, Muzny, Donna M., additional, Palli, Subba R., additional, Parisot, Nicolas, additional, Pick, Leslie, additional, Porter, Megan, additional, Qu, Jiaxin, additional, Refki, Peter N., additional, Richter, Rose, additional, Pomar, Rolando Rivera, additional, Rosendale, Andrew J., additional, Roth, Siegfried, additional, Sachs, Lena, additional, Santos, M. Emília, additional, Seibert, Jan, additional, Sghaier, Essia, additional, Shukla, Jayendra N., additional, Stancliffe, Richard J., additional, Tidswell, Olivia, additional, Traverso, Lucila, additional, Zee, Maurijn van der, additional, Viala, Séverine, additional, Worley, Kim C., additional, Zdobnov, Evgeny M., additional, Gibbs, Richard A., additional, and Richards, Stephen, additional

Published
2017
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74. Rates and delay times of Type Ia supernovae in the helium-enriched main-sequence donor scenario.

Author

Zheng-Wei Liu and Stancliffe, Richard J.

Subjects
TYPE I supernovae, MAIN sequence (Astronomy), BINARY stars, STELLAR evolution, STELLAR populations
Abstract

The nature of the progenitors of Type Ia supernovae (SNe Ia) remains a mystery. Comparing theoretical rates and delay-time distributions of SNe Ia with those inferred observationally can constrain their progenitor models. In this work, taking thermohaline mixing into account in the helium-enriched main-sequence (HEMS) donor scenario, we address rates and delay times of SNe Ia in this channel by combining the results of self-consistent binary evolution calculations with population synthesis models. We find that the Galactic SN Ia rate from the HEMS donor scenario is around 0.6-1.2 × 10-3 yr-1, which is about 30 per cent of the observed rate. Delay times of SNe Ia in this scenario cover a wide range of 0.1-1.0 Gyr. We also present the preexplosion properties of companion stars in the HEMS donor scenario, which will be helpful for placing constraints on SN Ia progenitors through analysing their pre-explosion images. [ABSTRACT FROM AUTHOR]

Published
2018
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76. CARBON-ENHANCED METAL-POOR STAR FREQUENCIES IN THE GALAXY: CORRECTIONS FOR THE EFFECT OF EVOLUTIONARY STATUS ON CARBON ABUNDANCES

Author

Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Frebel, Anna L., Placco, Vinicius M., Beers, Timothy C., Stancliffe, Richard J., Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Frebel, Anna L., Placco, Vinicius M., Beers, Timothy C., and Stancliffe, Richard J.

Abstract

We revisit the observed frequencies of carbon-enhanced metal-poor (CEMP) stars as a function of the metallicity in the Galaxy, using data from the literature with available high-resolution spectroscopy. Our analysis excludes stars exhibiting clear overabundances of neutron-capture elements and takes into account the expected depletion of surface carbon abundance that occurs due to CN processing on the upper red giant branch. This allows for the recovery of the initial carbon abundance of these stars, and thus for an accurate assessment of the frequencies of carbon-enhanced stars. The correction procedure we develop is based on stellar-evolution models and depends on the surface gravity, log g, of a given star. Our analysis indicates that for stars with [Fe/H] ≤–2.0, 20% exhibit [C/Fe] ≥+0.7. This fraction increases to 43% for [Fe/H] ≤–3.0 and 81% for [Fe/H] ≤–4.0, which is higher than have been previously inferred without taking the carbon abundance correction into account. These CEMP star frequencies provide important inputs for Galactic and stellar chemical evolution models, as they constrain the evolution of carbon at early times and the possible formation channels for the CEMP-no stars. We also have developed a public online tool with which carbon corrections using our procedure can be easily obtained., National Science Foundation (U.S.) (CAREER Grant AST-1255160)

Published
2015

82. Thermohaline mixing in low-mass giants: RGB and beyond

Author

Cantiello, M., Hoekstra, H., Langer, N., Poelarends, A.J.T., Stancliffe, Richard J., Astrophysics, Sub Astrophysics begr 1/1/14, Afd Astrophysics begr 1/1/17, and Dep Natuurkunde

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Physics::Geophysics
Abstract

Thermohaline mixing has recently been proposed to occur in low mass red giants, with large consequence for the chemical yields of low mass stars.We investigate the role of thermohaline mixing during the evolution of stars between 1M⊙ and 3M⊙, in comparison to other mixing processes acting in these stars. We use a stellar evolution code which includes rotational mixing and internal magnetic fields.We confirm that thermohaline mixing has the potential to destroy most of the 3He which is produced earlier on the main sequence during the red giant stage, in stars below 1.5M⊙.We find this process to continue during core helium burning and beyond.We find rotational and magnetic mixing to be negligible compared to the thermohaline mixing in the relevant layers, even if the interaction of thermohaline motions with the differential rotation may be essential to establish the time scale of thermohaline mixing in red giants.

Published
2007

83. Long GRBs from binary stars: runaway, Wolf-Rayet progenitors

Author

Cantiello, M., Yoon, S.C., Langer, N., Livio, M., Stancliffe, Richard J., Astrophysics, Sub Astrophysics begr 1/1/14, Dep Natuurkunde, and Afd Astrophysics begr 1/1/17

Abstract

The collapsar model for long gamma-ray bursts requires a rapidly rotating Wolf-Rayet star as progenitor. We test the idea of producing rapidly rotating Wolf-Rayet stars in massive close binaries through mass accretion and consecutive quasi-chemically homogeneous evolution — the latter had previously been shown to provide collapsars below a certain metallicity threshold for single stars. The binary channel presented here may provide a means for massive stars to obtain the high rotation rates required to evolve quasi-chemically homogeneous and fulfill the collapsar scenario. Moreover, it suggests that a possibly large fraction of long gamma-ray bursts occurs in runaway stars.

Published
2007

84. When stars collide

Author

Glebbeek, E., Pols, O.R., Stancliffe, Richard J., Astrophysics, Dep Natuurkunde, and Sub Astrophysics begr 1/1/14

Abstract

When two stars collide and merge they form a new star that can stand out against the background population in a star cluster as a blue straggler. In so called collision runaways many stars can merge and may form a very massive star that eventually forms an intermediate mass blackhole. We have performed detailed evolution calculations of merger remnants from collisions between main sequence stars, both for lower mass stars and higher mass stars. These stars can be significantly brighter than ordinary stars of the same mass due to their increased helium abundance. Simplified treatments ignoring this effect give incorrect predictions for the collision product lifetime and evolution in the Hertzsprung-Russell diagram.

Published
2007

85. Critically-rotating stars in binaries: an unsolved problem

Author

de Mink, S.E., Pols, O.R., Glebbeek, E., Stancliffe, Richard J., Astrophysics, Sub Astrophysics begr 1/1/14, and Dep Natuurkunde

Abstract

In close binaries mass and angular momentum can be transferred from one star to the other during Roche-lobe overflow. The efficiency of this process is not well understood and constitutes one of the largest uncertainties in binary evolution. One of the problems lies in the transfer of angular momentum, which will spin up the accreting star. In very tight systems tidal friction can prevent reaching critical rotation, by locking the spin period to the orbital period. Accreting stars in systems with orbital periods larger than a few days reach critical rotation after accreting only a fraction of their mass, unless there is an effective mechanism to get rid of angular momentum. In low-mass stars magnetic field might help. In more-massive stars angular-momentum loss will be accompanied by strong mass loss. This would imply that most interacting binaries with initial orbital periods larger than a few days evolve very non-conservatively. In this contribution we wish to draw attention to the unsolved problems related to mass and angular-momentum transfer in binary systems. We do this by presenting the first results of an implementation of spin up by accretion into the TWIN version of the Eggleton stellar-evolution code.

Published
2007

86. Can the helium-enriched main-sequence donor scenario hide enough hydrogen to explain Type Ia supernovae?

Author

Zheng-Wei Liu and Stancliffe, Richard J.

Subjects
TYPE I supernovae, HYDRODYNAMICS, BINARY stars, STELLAR evolution, MERIDIONAL overturning circulation
Abstract

Hydrodynamical simulations predict that a large amount of hydrogen (≥0.1 MΘ) is removed from a hydrogen-rich companion star by the SN explosion in the single-degenerate scenario of Type Ia supernovae (SNe Ia). However, non-detection of hydrogen-rich material in the late-time spectra of SNe Ia suggests that the hydrogen mass stripped from the progenitor system is ≤0.001-0.058 MΘ. In this Letter, we include thermohaline mixing into self-consistent binary evolution calculations for the helium-enriched main-sequence (HEMS) donor channel of SNe Ia for the first time. We find that the swept-up hydrogen masses expected in this channel are around 0.10-0.17 MΘ, which is higher than the observational limits, although the companion star is strongly helium-enriched when the SN explodes. This presents a serious challenge to the HEMS donor channel. [ABSTRACT FROM AUTHOR]

Published
2017
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88. METAL-POOR STARS OBSERVED WITH THE MAGELLAN TELESCOPE. I. CONSTRAINTS ON PROGENITOR MASS AND METALLICITY OF AGB STARS UNDERGOING s-PROCESS NUCLEOSYNTHESIS

Author

Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Frebel, Anna L., Placco, Vinicius M., Beers, Timothy C., Karakas, Amanda I., Kennedy, Catherine R., Rossi, Silvia, Christlieb, N., Stancliffe, Richard J., Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Frebel, Anna L., Placco, Vinicius M., Beers, Timothy C., Karakas, Amanda I., Kennedy, Catherine R., Rossi, Silvia, Christlieb, N., and Stancliffe, Richard J.

Abstract

We present a comprehensive abundance analysis of two newly discovered carbon-enhanced metal-poor (CEMP) stars. HE 2138?3336 is a s-process-rich star with [Fe/H] = -2.79, and has the highest [Pb/Fe] abundance ratio measured thus far, if non-local thermodynamic equilibrium corrections are included ([Pb/Fe] = +3.84). HE 2258?6358, with [Fe/H] = -2.67, exhibits enrichments in both s- and r-process elements. These stars were selected from a sample of candidate metal-poor stars from the Hamburg/ESO objective-prism survey, and followed up with medium-resolution (R ~ 2000) spectroscopy with GEMINI/GMOS. We report here on derived abundances (or limits) for a total of 34 elements in each star, based on high-resolution (R ~ 30, 000) spectroscopy obtained with Magellan-Clay/MIKE. Our results are compared to predictions from new theoretical asymptotic giant branch (AGB) nucleosynthesis models of 1.3? M [subscript ?] with [Fe/H] = ?2.5 and ?2.8, as well as to a set of AGB models of 1.0 to 6.0?M [subscript ?] at [Fe/H] = ?2.3. The agreement with the model predictions suggests that the neutron-capture material in HE 2138?3336 originated from mass transfer from a binary companion star that previously went through the AGB phase, whereas for HE 2258?6358, an additional process has to be taken into account to explain its abundance pattern. We find that a narrow range of progenitor masses (1.0 ? M(M [subscript ?]) ? 1.3) and metallicities (?2.8 ? [Fe/H] ??2.5) yield the best agreement with our observed elemental abundance patterns., National Science Foundation (U.S.)

Published
2014

92. SEVEN NEW CARBON-ENHANCED METAL-POOR RR LYRAE STARS

Author

Kennedy, Catherine R., primary, Stancliffe, Richard J., additional, Kuehn, Charles, additional, Beers, Timothy C., additional, Kinman, T. D., additional, Placco, Vinicius M., additional, Reggiani, Henrique, additional, Rossi, Silvia, additional, and Lee, Young Sun, additional

Published
2014
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93. Carbon-enhanced Metal-poor Stars and Thermohaline Mixing

Author

Stancliffe, Richard J., primary, Glebbeek, Evert, additional, Izzard, Robert G., additional, Pols, Onno R., additional, Stancliffe, Richard J., additional, Houdek, Guenter, additional, Martin, Rebecca G., additional, and Tout, Christopher A., additional

Published
2007
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98. Thermohaline mixing in low-mass giants: RGB and beyond

Author

Astrophysics, Sub Astrophysics begr 1/1/14, Afd Astrophysics begr 1/1/17, Dep Natuurkunde, Cantiello, M., Hoekstra, H., Langer, N., Poelarends, A.J.T., Stancliffe, Richard J., Astrophysics, Sub Astrophysics begr 1/1/14, Afd Astrophysics begr 1/1/17, Dep Natuurkunde, Cantiello, M., Hoekstra, H., Langer, N., Poelarends, A.J.T., and Stancliffe, Richard J.

Published
2007

99. When stars collide

Author

Astrophysics, Dep Natuurkunde, Sub Astrophysics begr 1/1/14, Glebbeek, E., Pols, O.R., Stancliffe, Richard J., Astrophysics, Dep Natuurkunde, Sub Astrophysics begr 1/1/14, Glebbeek, E., Pols, O.R., and Stancliffe, Richard J.

Published
2007

100. Long GRBs from binary stars: runaway, Wolf-Rayet progenitors

Author

Astrophysics, Sub Astrophysics begr 1/1/14, Dep Natuurkunde, Afd Astrophysics begr 1/1/17, Cantiello, M., Yoon, S.C., Langer, N., Livio, M., Stancliffe, Richard J., Astrophysics, Sub Astrophysics begr 1/1/14, Dep Natuurkunde, Afd Astrophysics begr 1/1/17, Cantiello, M., Yoon, S.C., Langer, N., Livio, M., and Stancliffe, Richard J.

Published
2007

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