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Your search keyword '"Kiss, Laszlo L."' showing total 5 results
Start Over Author "Kiss, Laszlo L." Topic fos: physical sciences
5 results on '"Kiss, Laszlo L."'

1. The peak-flux of GRB 221009A measured with GRBAlpha

Author

Ripa, Jakub, Takahashi, Hiromitsu, Fukazawa, Yasushi, Werner, Norbert, Munz, Filip, Pal, Andras, Ohno, Masanori, Dafcikova, Marianna, Meszaros, Laszlo, Csak, Balazs, Husarikova, Nikola, Kolar, Martin, Galgoczi, Gabor, Breuer, Jean-Paul, Hroch, Filip, Hudec, Jan, Kapus, Jakub, Frajt, Marcel, Rezenov, Maksim, Laszlo, Robert, Koleda, Martin, Smelko, Miroslav, Hanak, Peter, Lipovsky, Pavol, Urbanec, Tomas, Kasal, Miroslav, Povalac, Ales, Uchida, Yuusuke, Poon, Helen, Matake, Hiroto, Nakazawa, Kazuhiro, Uchida, Nagomi, Bozoki, Tamas, Dalya, Gergely, Enoto, Teruaki, Frei, Zsolt, Friss, Gergely, Ichinohe, Yuto, Kapas, Kornel, Kiss, Laszlo L., Mizuno, Tsunefumi, Odaka, Hirokazu, Takatsy, Janos, Topinka, Martin, and Torigoe, Kento

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The brightest gamma-ray burst ever observed, long-duration GRB 221009A, was detected by GRBAlpha nano-satellite without saturation. We present light curves of the prompt emission in 13 energy bands, from 80 keV to 950 keV, and perform a spectral analysis to calculate the peak flux and peak isotropic-equivalent luminosity. Since the satellite's attitude information is not available for the time of this GRB, more than 200 incident directions were probed in order to find the median luminosity and its systematic uncertainty. We found that the peak flux in the $80-800$ keV range (observer frame) was $F_{\rm{ph}}^{\rm{p}}=1300_{-200}^{+1200}$ ph cm$^{-2}$s$^{-1}$ or $F_{\rm{erg}}^{\rm{p}}=5.7_{-0.7}^{+3.7}\times10^{-4}$ erg cm$^{-2}$s$^{-1}$ and the fluence in the same energy range of the first GRB episode lasting 300 s, which was observable by GRBAlpha, was $S=2.2_{-0.3}^{+1.4}\times10^{-2}$ erg cm$^{-2}$ or $S^{\rm{bol}}=4.9_{-0.5}^{+0.8}\times10^{-2}$ erg cm$^{-2}$ for the extrapolated range of $0.9-8,690$ keV. We infer the isotropic-equivalent released energy of the first GRB episode to be $E_{\rm{iso}}^{\rm{bol}}=2.8_{-0.5}^{+0.8}\times10^{54}$ erg in the $1-10,000$ keV band (rest frame at $z=0.15$). The peak isotropic-equivalent luminosity in the $92-920$ keV range (rest frame) was $L_{\rm{iso}}^{\rm{p}}=3.7_{-0.5}^{+2.5}\times10^{52}$ erg s$^{-1}$ and the bolometric peak isotropic-equivalent luminosity was $L_{\rm{iso}}^{\rm{p,bol}}=8.4_{-1.5}^{+2.5}\times10^{52}$ erg s$^{-1}$ (4 s scale) in the $1-10,000$ keV range (rest frame). The peak emitted energy is $E_p^\ast=E_p(1+z)=1120\pm470$ keV. Our measurement of $L_{\rm{iso}}^{\rm{p,bol}}$ is consistent with the Yonetoku relation. It is possible that, due to the spectral evolution of this GRB and orientation of GRBAlpha at the peak time, the true values of peak flux, fluence, $L_{\rm{iso}}$, and $E_{\rm{iso}}$ are even higher. [abridged], 7 pages, 7 figures, 1 table, accepted for publication in Astronomy & Astrophysics

Published
2023

2. TOI-836: A super-Earth and mini-Neptune transiting a nearby K-dwarf

Author

Hawthorn, Faith, Bayliss, Daniel, Wilson, Thomas G, Bonfanti, Andrea, Adibekyan, Vardan, Alibert, Yann, Sousa, Sérgio G, Collins, Karen A, Bryant, Edward M, Osborn, Ares, Armstrong, David J, Abe, Lyu, Acton, Jack S, Addison, Brett C, Agabi, Karim, Alonso, Roi, Alves, Douglas R, Anglada-Escudé, Guillem, Bárczy, Tamas, Barclay, Thomas, Barrado, David, Barros, Susana C C, Baumjohann, Wolfgang, Bendjoya, Philippe, Benz, Willy, Bieryla, Allyson, Bonfils, Xavier, Bouchy, François, Brandeker, Alexis, Broeg, Christopher, Brown, David J A, Burleigh, Matthew R, Buttu, Marco, Cabrera, Juan, Caldwell, Douglas A, Casewell, Sarah L, Charbonneau, David, Charnoz, Sébastian, Cloutier, Ryan, Cameron, Andrew Collier, Collins, Kevin I, Conti, Dennis M, Crouzet, Nicolas, Czismadia, Szilárd, Davies, Melvyn B, Deleuil, Magali, Delgado-Mena, Elisa, Delrez, Laetitia, Demangeon, Olivier D S, Demory, Brice-Olivier, Dransfield, Georgina, Dumusque, Xavier, Egger, Jo Ann, Ehrenreich, David, Eigmüller, Philipp, Erickson, Anders, Essack, Zahra, Fortier, Andrea, Fossati, Luca, Fridlund, Malcolm, Günther, Maximilian N, Güdel, Manuel, Gandolfi, Davide, Gillard, Harvey, Gillon, Michaël, Gnilka, Crystal, Goad, Michael R, Goeke, Robert F, Guillot, Tristan, Hadjigeorghiou, Andreas, Hellier, Coel, Henderson, Beth A, Heng, Kevin, Hooton, Matthew J, Horne, Keith, Howell, Steve B, Hoyer, Sergio, Irwin, Jonathan M, Jenkins, James S, Jenkins, Jon M, Jensen, Eric L N, Kane, Stephen R, Kendall, Alicia, Kielkopf, John F, Kiss, Laszlo L, Lacedelli, Gaia, Laskar, Jacques, Latham, David W, Etangs, Alain Lecavalier des, Leleu, Adrien, Lendl, Monika, Lillo-Box, Jorge, Lovis, Christophe, Mékarnia, Djamel, Massey, Bob, Masters, Tamzin, Maxted, Pierre F L, Nascimbeni, Valerio, Nielsen, Louise D, O’Brien, Sean M, Olofsson, Göran, Osborn, Hugh Patrick, Pagano, Isabella, Pallé, Enric, Persson, Carina M, Piotto, Giampaolo, Plavchan, Peter, Pollacco, Don, Queloz, Didier, Ragazzoni, Roberto, Rauer, Heike, Ribas, Ignasi, Ricker, George, Ségransan, Damien, Salmon, Sébastien, Santerne, Alexandre, Santos, Nuno C, Scandariato, Gaetano, Schmider, François-Xavier, Schwarz, Richard P, Seager, Sara, Shporer, Avi, Simon, Attila, Smith, Alexis M S, Srdoc, Gregor, Steller, Manfred, Suarez, Olga, Szabó, Gyula M, Teske, Johanna, Thomas, Nicolas, Tilbrook, Rosanna H, Triaud, Amaury H M J, Udry, Stéphane, Van Grootel, Valérie, Walton, Nicholas, Wang, Sharon X, Wheatley, Peter J, Winn, Joshua N, Wittenmyer, Robert A, Zhang, Hui, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Astrophysique de Marseille (LAM), 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), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
planets and satellites: detection, 530 Physics, individual: TOI-836 ((TIC 440887364, GAIA EDR3 6230733559097425152) [Stars], FOS: Physical sciences, 610 Medicine & health, techniques: photometric, techniques: radial velocities, QB Astronomy, QC, QB, MCC, Earth and Planetary Astrophysics (astro-ph.EP), radial velocities [Techniques], 520 Astronomy, photometric [Techniques], GAIA EDR3 6230733559097425152), Astronomy and Astrophysics, DAS, 620 Engineering, detection [Planets and satellites], QC Physics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], 570 Life sciences, biology, stars: individual: TOI-836 (TIC 440887364, Astrophysics - Earth and Planetary Astrophysics
Abstract

Funding: TGW, ACC, and KH acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant ST/R003203/1. We present the discovery of two exoplanets transiting TOI-836 (TIC 440887364) using data from TESS Sector 11 and Sector 38. TOI-836 is a bright (T = 8.5 mag), high proper motion (∼200 mas yr−1), low metallicity ([Fe/H]≈−0.28) K-dwarf with a mass of 0.68 ± 0.05 M⊙ and a radius of 0.67 ± 0.01 R⊙. We obtain photometric follow-up observations with a variety of facilities, and we use these data-sets to determine that the inner planet, TOI-836 b, is a 1.70 ± 0.07 R⊕ super-Earth in a 3.82 day orbit, placing it directly within the so-called ‘radius valley’. The outer planet, TOI-836 c, is a 2.59 ± 0.09 R⊕ mini-Neptune in an 8.60 day orbit. Radial velocity measurements reveal that TOI-836 b has a mass of 4.5 ± 0.9 M⊕, while TOI-836 c has a mass of 9.6 ± 2.6 M⊕. Photometric observations show Transit Timing Variations (TTVs) on the order of 20 minutes for TOI-836 c, although there are no detectable TTVs for TOI-836 b. The TTVs of planet TOI-836 c may be caused by an undetected exterior planet. Publisher PDF

Published
2023

3. The gamma-ray binary LS 5039: mass and orbit constraints from MOST observations

Author

Sarty, Gordon E., Szalai, Tamas, Kiss, Laszlo L., Matthews, Jaymie M., Wu, Kinwah, Kuschnig, Rainer, Guenther, David B., Moffat, Anthony F. J., Rucinski, Slavek M., Sasselov, Dimitar, Weiss, Werner W., Huziak, Richard, Johnston, Helen M., Phillips, Andre, and Ashley, Michael C. B.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

The results of a coordinated space-based photometric and ground-based spectroscopic observing campaign on the enigmatic gamma-ray binary LS 5039 are reported. Sixteen days of observations from the MOST satellite have been combined with high-resolution optical echelle spectroscopy from the 2.3m ANU Telescope in Siding Spring, Australia. These observations were used to measure the orbital parameters of the binary and to study the properties of stellar wind from the O primary. We found that any broad-band optical photometric variability at the orbital period is below the 2 mmag level, supporting the scenario that the orbital eccentricity of the system is near the 0.24 +/- 0.08 value implied by our spectroscopy, which is lower than values previously obtained by other workers. The low amplitude optical variability also implies the component masses are at the higher end of estimates based on the primary's O6.5V((f)) spectral type with a primary mass of ~26 solar masses and a mass for the compact star of at least 1.8 solar masses. The mass loss rate from the O primary was determined to be 3.7E-7 to 4.8E-7 solar masses per year., Accepted for MNRAS 2010 September 22

Published
2010

4. Finding Periods in High Mass X-Ray Binaries

Author

Sarty, Gordon E., Kiss, Laszlo L., Johnston, Helen M., Huziak, Richard, and Wu, Kinwah

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

This is a call for amateur astronomers who have the equipment and experience for producing high quality photometry to contribute to a program of finding periods in the optical light curves of high mass X-ray binaries (HMXB). HMXBs are binary stars in which the lighter star is a neutron star or a black hole and the more massive star is an O type supergiant or a Be type main sequence star. Matter is transferred from the ordinary star to the compact object and X-rays are produced as the the gravitational energy of the accreting gas is converted into light. HMXBs are very bright, many are brighter than 10th magnitude, and so make perfect targets for experienced amateur astronomers with photometry capable CCD equipment coupled with almost any size telescope., Accepted: JAAVSO

Published
2007

5. Solar-like oscillations in alpha Centauri B

Author

Kjeldsen, Hans, Bedding, Timothy R., Butler, R. Paul, Christensen-Dalsgaard, Joergen, Kiss, Laszlo L., McCarthy, Chris, Marcy, Geoffrey W., Tinney, Christopher G., and Wright, Jason T.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics
Abstract

We have made velocity observations of the star alpha Cen B from two sites, allowing us to identify 37 oscillation modes with l=0-3. Fitting to these modes gives the large and small frequency separations as a function of frequency. The mode lifetime, as measured from the scatter of the oscillation frequencies about a smooth trend, is similar to that in the Sun. Limited observations of the star delta Pav show oscillations centred at 2.3 mHz with peak amplitudes close to solar. We introduce a new method of measuring oscillation amplitudes from heavily-smoothed power density spectra, from which we estimated amplitudes for alpha Cen A and B, beta Hyi, delta Pav and the Sun. We point out that the oscillation amplitudes may depend on which spectral lines are used for the velocity measurements., accepted for publication in ApJ

Published
2005

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