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What Asteroseismology Can Do for Exoplanets: Kepler-410A B Is a Small Neptune Around a Bright Star, in an Eccentric Orbit Consistent with Low Obliquity
What asteroseismology can do for exoplanets: Kepler-410A b is a Small Neptune around a bright star, in an eccentric orbit consistent with low obliquity V. Van Eylen1;2?, M. N. Lund1;4, V. Silva Aguirre1, T. Arentoft1, H. Kjeldsen1, S. Albrecht3, W. J. Chaplin5, H. Isaacson6, M. G. Pedersen1, J. Jessen-Hansen1, B. Tingley1, J. Christensen-Dalsgaard1, C. Aerts2, T. L. Campante5 and S. T. Bryson7 1 Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark 2 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Heverlee, Belgium 3 Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 4 Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia 5 School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham, B15 2TT, UK 6 Department of Astronomy, University of California, Berkeley, CA 94820, USA 7 NASA Ames Research Center, Moffett Field, CA 94035 [email protected] ABSTRACT We confirm the Kepler planet candidate Kepler-410b (KOI-42b) as a Neptune sized exoplanet on a 17:8 day, eccentric orbit around the bright (Kp = 9:4) star Kepler-410A. This is the third brightest confirmed planet host star in the Kepler field and one of the brightest hosts of all currently known transiting exoplanets. Kepler-410 consists of a blend between the fast rotat- ing planet host star (Kepler-410A) and a fainter star (Kepler-410B), which has complicated the confirmation of the planetary candidate. -
What Asteroseismology Can Do for Exoplanets: KOI-42Ab Is a Small Neptune in an Eccentric Orbit Consistent with Low Obliquity
What asteroseismology can do for exoplanets: KOI-42Ab is a Small Neptune in an eccentric orbit consistent with low obliquity V. Van Eylen1;2?, M. N. Lund1;4, V. Silva Aguirre1, T. Arentoft1, H. Kjeldsen1, S. Albrecht3, W. J. Chaplin5, H. Isaacson6, M. G. Pedersen1, J. Jessen-Hansen1, B. Tingley1, J. Christensen-Dalsgaard1, C. Aerts2 and T. Campante5 1 Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark 2 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Heverlee, Belgium 3 Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 4Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia 5School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham, B15 2TT, UK 6Department of Astronomy, University of California, Berkeley, CA 94820, USA [email protected] ABSTRACT We confirm the Kepler planet candidate KOI-42b as a Neptune sized exoplanet on a 17:8 day, eccentric, orbit around the bright (Kp = 9:4) star KOI-42A. KOI-42 consists of a blend between the fast rotating planet host star (KOI-42A) and a fainter star (KOI-42B), which has complicated the confirmation of the planetary candidate. Employing asteroseismology, using constraints from the transit light curve, adaptive optics and speckle images, and Spitzer transit observations, we demonstrate that the candidate can only be an exoplanet orbiting KOI-42A. Via asteroseismology we determine the following stellar and planetary parameters with high precision; M? = 1:214 ± 0:033 M ,R? = 1:352 ± 0:010 R , Age = 2:76 ± 0:54 Gyr, planetary radius (2:838 ± 0:054 R⊕), and +0:10 orbital eccentricity (0:17−0:05). -
Transit Timing Variations, Radial Velocities and Long-Term Dynamical Stability of the System Kepler-410?
MNRAS 484, 4352{4359 (2019) Preprint 12th February 2019 Compiled using MNRAS LATEX style file v3.0 Transit timing variations, radial velocities and long-term dynamical stability of the system Kepler-410? Pavol Gajdoˇs1†, Martin Vaˇnko2, Theodor Pribulla2, Daniel Dupkala3,4, J´an Subjakˇ 3,4, Marek Skarka3,5, Petr Kab´ath3, L'ubom´ır Hamb´alek2, Stefanˇ Parimucha1 1Institute of Physics, Faculty of Science, Pavol Jozef Saf´arikˇ University, Koˇsice, Slovakia 2Astronomical Institute, Slovak Academy of Sciences, 059 60 Tatransk´aLomnica, Slovakia 3Astronomical Institute, Czech Academy of Sciences, Friˇcova 298, 25165, Ondˇrejov, Czech Republic 4Astronomical Institute of Charles University, V Holeˇsoviˇck´ach 2, 180 00, Praha, Czech Republic 5Department of Theoretical Physics and Astrophysics, Masaryk Univerzity, Kotl´aˇrsk´a2, 61137 Brno, Czech Republic Accepted 2019 January 22. Received 2019 January 21; in original form 2018 December 14. ABSTRACT Transit timing variations of Kepler-410Ab were already reported in a few papers. Their semi-amplitude is about 14.5 minutes. In our previous paper, we found that the transit timing variations could be caused by the presence of a stellar companion in this system. Our main motivation for this paper was to investigate variation in a radial-velocity curve generated by this additional star in the system. We performed spectroscopic observation of Kepler-410 using three telescopes in Slovakia and Czech Republic. Using the cross-correlation function, we measured the radial velocities of the star Kepler-410A. We did not observe any periodic variation in a radial-velocity curve. Therefore, we rejected our previous hypothesis about additional stellar companion in the Kepler-410 system. -
Cosmic Noise: a History of Early Radio Astronomy Woodruff T
Cambridge University Press 978-0-521-76524-4 - Cosmic Noise: A History of Early Radio Astronomy Woodruff T. Sullivan Index More information Index A bold number indicates the most important page(s) An italicized number indicates that a figure is included in the page(s) Acuff, Roy versus Ludwig van Beethoven animals (cont.) Aron, Raymond 13 265 eagle 277 Ashkhabad, Turkmenistan 238 Adel, Arthur 86, 98 elephant 374 Aspinall, Arnold 243–5 Adgie, Ronald 173 fish 168 Astapovich, I. S. 238 Admiralty Signal Establishment (UK) flea 480 astronomers 115, 156, 264, 288 giraffe 317 amateur 41, 74–5, 182–3, 241, 247, 265 Agassiz, Louis 91 gnat 374 relations with radio researchers 47–9, Air Defence Research and Development goose 258 75–6, 138, 152, 175, 182, 195–6, Establishment (UK) 156 gorilla 39 224, 253, 313, 404, 416, 425, 435, Alexander, F. Elizabeth S. 85, 128–9, 319 horse 168, 376, 446 439–41, 452, Alfvén, Hannes 309, 374, 386 hydra 39 astronomical (term) 425–6 synchrotron radiation for radio stars mongoose 389 astronomies, beginnings of various 379–80 monkey 279 wavelength bands 451, 462–7 Allen, Clabon W. “Cla” 130, 132, 137, octopus 346 astronomy 288, 297, 425, 426, 430 rabbit 279 extreme ultraviolet 464 Allen, E. W., Jr. 257 serpent 39 gamma ray 391, 464 All-India Radio 256 swan 142 high energy 384, 389–91 Almond, Mary 245, 248–50 tadpole 256 infrared 428, 463 Altar, Wilhelm 91 trout 32 optical 384, 424, 427–9 Alvin 455 turkey 32 comparison with radio astronomy Amalgamated Wireless Australasia, Ltd. -
Proceedings of the 29 Grain Formation Workshop / Dust In
Proceedings of the 29th Grain Formation Workshop / Dust in Galaxies 2011 held at Center of Planetary Science (CPS), Kobe, Japan 9—11 November 2011 Eds.: S. Okuzumi, I. Sakon, Y. Kimura, A. Inoue, H. Kimura, H. Miura, T. Muto, T. Yamamoto Online materials; https://www.cps-jp.org/~gfw/pub/2011-11-09/ 1 Proceedings of the 29th Grain Formation Workshop / Dust in Galaxies 2011 held at Center of Planetary Science (CPS), Kobe, Japan 9—11 November 2011 Eds.: S. Okuzumi, I. Sakon, Y. Kimura, A. Inoue, H. Kimura, H. Miura, T. Muto, T. Yamamoto Online materials; https://www.cps-jp.org/~gfw/pub/2011-11-09/ 2 Program 9th November, 2011 13:30-13:40 Tetsuo Yamamoto (Hokkaido University) / Akio Inoue (Osaka Sangyo University) “Opening Remarks” 13:40-14:00 Akemi Tamanai (Heidelberg University) “A study of dust grain formation: A role of minor elements” 14:00-14:20 Chiyoe Koike (Osaka University) “IR spectra of silica (SiO2) polymorphs” 14:20-14:40 Steffen Wetzel (Heidelberg University) “Condensation and solid phase reactions of Mg silicate system” (coffee break) 15:00-15:40 Aki Takigawa (University of Tokyo) “Morphological analyses of presolar alumina grains towards understanding the circumstellar dust formation and evolution processes” 15:40-16:00 Yuki Kimura (Tohoku University) “Homogeneous nucleation experiment of cosmic dust” (coffee break) 16:20-16:40 Akane Sakurai (Nagoya university) “Star formation and dust extinction properties of local galaxies seen from AKARI” 16:40-17:00 Tsutomu Takeuchi (Nagoya University) “A Study on the Star Formation History