DOCSLIB.ORG

972 Stars in Different Stages of Metamorphosis Jupiter Radius

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
972 Stars in Different Stages of Metamorphosis Jupiter Radius 972 Stars in Different Stages of Metamorphosis Jeffrey J. Wolynski October 6, 2018 Rockledge, FL 32955 Abstract: A simple graph is provided on log10 scale for masses that young hot stars become colder older smaller stars, mislabeled "planets/brown dwarfs/exoplanets" by the establishment. The data is freely available online and is sourced in this paper. The graph is self-explanatory, stars lose mass and shrink on a continuous basis, becoming life hosting worlds to the bottom left, after billions of years of evolutionary sequences. The radii and masses of the stars are referenced against Jupiter, as Jupiter is a good middle ground star just exiting its brown dwarf stages of evolution, but not too evolved as to host life as of yet. This graph will be strengthened more when the TESS data comes back, and the author includes even more brown dwarfs that are already directly observed. I can't remember who said it, but the authority of 10,000 is no match against the simple reasoning of a single individual. The book of stellar metamorphosis: http://vixra.org/pdf/1711.0206v3.pdf 972 Stars in Different Stages of Metamorphosis 6250 125 2.5 0 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 34 35 36 Jupiter Masses Jupiter 0.05 0.001 Jupiter Radius Star Radius Mass Kepler-138b 0.047 0.00021 Kepler-453b 0.553 0.00063 TRAPPIST-1d 0.069 0.00129 Kepler-70b 0.068 0.0014 TRAPPIST-1e 0.082 0.00195 Kepler-138d 0.108 0.00201 Kepler-70c 0.077 0.0021 TRAPPIST-1f 0.093 0.00214 TRAPPIST-1b 0.097 0.00267 K2-239c 0.089 0.0028 Earth 0.09 0.003 K2-239d 0.098 0.0041 TRAPPIST-1g 0.101 0.00422 TRAPPIST-1c 0.094 0.00434 K2-239b 0.098 0.0044 Gliese 1132 b 0.103 0.0051 Kepler-78b 0.105 0.006 Kepler-11b 0.161 0.006 Kepler-11f 0.222 0.006 Kepler-177b 0.259 0.006 Kepler-138c 0.107 0.0062 Kepler-51b 0.633 0.007 K2-229b 0.102 0.0082 Kepler-406c 0.076 0.009 Kepler-114c 0.143 0.009 Kepler-11c 0.256 0.009 Kepler-101c 0.112 0.01 Kepler-414b 0.153 0.011 Kepler-307c 0.196 0.01145 Kepler-114d 0.226 0.012 Kepler-60c 0.17 0.01211 Kepler-48b 0.168 0.0124 Kepler-29c 0.28 0.01259 Kepler-80e 0.143 0.01299 Kepler-62c 0.048 0.013 Kepler-289d 0.239 0.013 Kepler-79e 0.311 0.013 Kepler-51c 0.803 0.013 Kepler-60d 0.178 0.01309 Kepler-60b 0.153 0.01318 HD 219134 c 0.135 0.01372 Kepler-36b 0.133 0.014 K2-240c 0.16 0.014 Kepler-29b 0.299 0.01419 Kepler-105c 0.117 0.01447 Kepler-10b 0.132 0.0145 HD 219134 b 0.143 0.01491 K2-155b 0.138 0.015 K2-155d 0.146 0.015 Kepler-223e 0.41 0.0151 Kepler-21b 0.146 0.01598 K2-141b 0.135 0.016 K2-240b 0.18 0.016 Kepler-1655b 0.1974 0.016 Kepler-223c 0.307 0.01605 Kepler-26b 0.248 0.01611 K2-131b 0.152 0.017 COROT-7b 0.141 0.018 COROT-24b 0.33 0.018 Kepler-68b 0.208 0.01878 Kepler-99b 0.132 0.019 Kepler-92c 0.232 0.019 Kepler-350c 0.277 0.019 Kepler-305c 0.294 0.019 Kepler-79c 0.332 0.019 Kepler-79d 0.639 0.019 Kepler-26c 0.243 0.01951 Gliese 1214 b 0.254 0.0197 Kepler-406b 0.128 0.02 K2-155c 0.174 0.02 Kepler-87c 0.548 0.02 LHS 1140 b 0.128 0.0209 Kepler-80c 0.244 0.02121 Kepler-80d 0.136 0.02124 Kepler-454b 0.211 0.02152 Kepler-80b 0.238 0.0218 Kepler-18b 0.178 0.022 Kepler-68c 0.089 0.02265 HD 219134 f 0.117 0.02297 Kepler-100b 0.118 0.023 Kepler-289b 0.192 0.023 Kepler-11d 0.278 0.023 K2-141c 0.624 0.023 Kepler-223b 0.267 0.02328 Kepler-307b 0.217 0.02341 Kepler-177c 0.633 0.024 Kepler-51d 0.865 0.024 HD 97658 b 0.209 0.02473 Kepler-48d 0.182 0.025 Kepler-36c 0.328 0.025 Kepler-11e 0.374 0.025 Kepler-223d 0.467 0.02517 55 Cancri e 0.17 0.02542 HD 106315 b 0.207 0.0255 Kepler-131c 0.075 0.026 K2-106b 0.136 0.0263 Kepler-338e 0.139 0.027 Kepler-88b 0.337 0.027 K2-111b 0.17 0.0271 Kepler-102e 0.198 0.028 WASP-47e 0.162 0.02863 Kepler-62b 0.117 0.03 Kepler-25b 0.242 0.0302 Kepler-20b 0.167 0.03052 Kepler-103b 0.301 0.031 K2-38c 0.216 0.03115 Kepler-37b 0.029 0.03146 Kepler-20d 0.245 0.03168 K2-32d 0.306 0.03241 Kepler-89b 0.153 0.033 Kepler-106c 0.223 0.033 Kepler-305b 0.321 0.033 Kepler-79b 0.31 0.0343 K2-95b 0.31 0.03458 Kepler-417b 0.206 0.035 Kepler-106e 0.228 0.035 Kepler-30b 0.348 0.036 Kepler-113b 0.162 0.037 HIP 116454 b 0.226 0.037 Kepler-37c 0.067 0.03776 K2-38b 0.138 0.03776 COROT-22b 0.435 0.038 K2-32c 0.269 0.03807 Kepler-37d 0.173 0.03839 Kepler-20c 0.272 0.04012 Kepler-238f 0.178 0.042 Gliese 3470 b 0.346 0.043 Kepler-62d 0.174 0.044 Kepler-48c 0.242 0.04597 Kepler-350d 0.25 0.047 Kepler-89c 0.385 0.049 HD 219134 d 0.144 0.05088 Kepler-131b 0.215 0.051 Kepler-276d 0.25 0.051 BD+20 594 b 0.199 0.05129 K2-32b 0.458 0.05191 Kepler-276c 0.259 0.052 Kepler-18d 0.623 0.052 K2-110b 0.2312 0.0525 WASP-47d 0.331 0.05286 Kepler-10c 0.21 0.054 Neptune 0.346 0.054 Kepler-18c 0.49 0.054 HD 106315 c 0.385 0.056 Kepler-396c 0.473 0.056 HAT-P-26b 0.565 0.059 Kepler-19b 0.197 0.064 K2-229c 0.181 0.067 Gliese 436 b 0.372 0.07 Kepler-56b 0.581 0.07 Kepler-30d 0.785 0.073 Kepler-4b 0.357 0.077 Kepler-25c 0.464 0.0774 Kepler-11g 0.297 0.079 HAT-P-11b 0.422 0.081 K2-10b 0.343 0.08495 K2-236b 0.546 0.085 COROT-24c 0.44 0.088 Kepler-328b 0.205 0.09 Kepler-414c 0.269 0.094 Kepler-117b 0.719 0.094 K2-105b 0.369 0.09439 Kepler-128b 0.101 0.097 K2-27b 0.4 0.09722 K2-98b 0.384 0.10131 Kepler-128c 0.101 0.105 Kepler-62f 0.126 0.11 Kepler-89e 0.585 0.11 HD 89345 b 0.66 0.11 Kepler-62e 0.144 0.113 Kepler-122f 0.156 0.113 Kepler-22b 0.212 0.113 Kepler-103c 0.459 0.114 Kepler-145b 0.236 0.117 WASP-139b 0.8 0.117 Kepler-279d 0.277 0.118 HATS-7b 0.563 0.12 WASP-107b 0.94 0.12 Kepler-328c 0.482 0.124 K2-39b 0.509 0.12522 Kepler-35b 0.728 0.127 WASP-156b 0.51 0.128 HATS-8b 0.873 0.138 CoRoT 223977153 b 0.57 0.15 Kepler-279c 0.384 0.155 Kepler-101b 0.51 0.16 Kepler-9c 0.823 0.171 HATS-46b 0.903 0.173 Kepler-282e 0.277 0.177 WASP-127b 1.37 0.18 Kepler-416b 0.221 0.183 K2-108b 0.471 0.18689 Kepler-282d 0.219 0.192 KELT-11b 1.37 0.195 HAT-P-18b 0.995 0.197 Kepler-277c 0.3 0.202 Kepler-92b 0.313 0.202 Kepler-413b 0.388 0.211 HAT-P-12b 0.959 0.211 K2-140b 1.093 0.211 COROT-8b 0.57 0.22 Kepler-34b 0.764 0.22 K2-261b 0.85 0.223 HATS-5b 0.912 0.237 Kepler-396b 0.312 0.238 WASP-29b 0.792 0.244 Kepler-145c 0.385 0.25 Kepler-425b 0.978 0.25 Kepler-9b 0.842 0.252 WASP-69b 1.057 0.26 HATS-43b 1.18 0.261 HAT-P-38b 0.825 0.267 COROT-25b 1.08 0.27 WASP-131b 1.22 0.27 Kepler-277b 0.261 0.275 WASP-117b 1.021 0.2755 WASP-126b 0.96 0.28 WASP-39b 1.27 0.28 Kepler-427b 1.23 0.29 HAT-P-19b 1.132 0.292 WASP-83b 1.04 0.3 WASP-21b 1.07 0.3 HAT-P-51b 1.293 0.309 WASP-151b 1.13 0.31 WASP-20b 1.462 0.311 HATS-6b 0.998 0.319 Kepler-16b 0.754 0.333 Kepler-89d 1.005 0.334 Kepler-426b 1.09 0.34 HAT-P-67b 2.085 0.34 HAT-P-44b 1.242 0.352 HD 149026 b 0.813 0.368 Kepler-54c 0.11 0.37 Kepler-415b 0.108 0.377 Kepler-63b 0.545 0.378 WASP-49b 1.115 0.378 WASP-63b 1.43 0.38 Kepler-38b 0.384 0.384 K2-139b 0.808 0.387 HATS-50b 1.13 0.39 WASP-153b 1.55 0.39 K2-232b 1 0.398 HD 63454 b 1.098 0.398 WASP-132b 0.87 0.41 Kepler-289c 1.034 0.42 WASP-67b 1.4 0.42 K2-60b 0.683 0.426 Kepler-77b 0.96 0.43 Kepler-422b 1.15 0.43 Kepler-12b 1.754 0.432 Wasp 144 b 0.85 0.44 Kepler-7b 1.622 0.441 KELT-6b 1.18 0.442 WASP-94Ab 1.72 0.452 WASP-52b 1.27 0.46 COROT-5b 1.388 0.467 WASP-113b 1.409 0.475 WASP-13b 1.389 0.477 WASP-31b 1.549 0.478 WASP-96b 1.2 0.48 COROT-28b 0.955 0.484 WASP-6b 1.23 0.485 WASP-17b 1.991 0.486 WASP-11b 1.005 0.487 HAT-P-46b 1.284 0.493 TrES-4b 1.838 0.494 Kepler-32c 0.178 0.5 WASP-101b 1.41 0.5 Kepler-45b 0.96 0.505 WASP-60b 0.86 0.514 WASP-118b 1.44 0.514 COROT-26b 1.26 0.52 HAT-P-1b 1.319 0.525 HATS-10b 0.969 0.526 WASP-42b 1.122 0.527 HAT-P-65b 1.89 0.527 HATS-27b 1.5 0.53 PH1b 0.551 0.531 Kepler-238e 0.5 0.534 HAT-P-17b 1.01 0.534 COROT-16b 1.17 0.535 WASP-80b 0.999 0.538 WASP-15b 1.428 0.542 HATS-13b 1.212 0.543 HATS-44b 1.067 0.56 Kepler-41b 1.29 0.56 WASP-88b 1.7 0.56 HAT-P-25b 1.19 0.567 Kepler-56c 0.874 0.57 WASP-62b 1.39 0.57 WASP-56b 1.092 0.571 WASP-157b 1.065 0.574 K2-30b 1.039 0.579 WASP-25b 1.22 0.58 HAT-P-55b 1.182 0.582 WASP-70Ab 1.164 0.59 WASP-34b 1.22 0.59 Kepler-8b 1.416 0.59 HAT-P-3b 0.827 0.591 Kepler-423b 1.192 0.595 HATS-53b 1.34 0.595 XO-2Nb 1.019 0.597 HAT-P-39b 1.571 0.599 WASP-124b 1.24 0.6 HATS-25b 1.26 0.613 HAT-P-40b 1.73 0.615 WASP-22b 1.199 0.617 HAT-P-27b 1.02 0.62 OGLE-TR-10b 1.25 0.62 HAT-P-28b 1.212 0.626 WASP-55b 1.335 0.627 Kepler-74b 0.96 0.63 HATS-39b 1.57 0.63 WASP-90b 1.63 0.63 WASP-54b 1.653 0.636 WASP-57b 1.05 0.644 HATS-26b 1.75 0.65 HATS-29b 1.251 0.653 Kepler-15b 0.96 0.66 HAT-P-43b 1.281 0.662 Kepler-6b 1.304 0.668 HAT-P-4b 1.274 0.671 HATS-28b 1.194 0.672 KELT-10b 1.399 0.679 HAT-P-24b 1.242 0.685 WASP-84b 0.942 0.694 HATS-45b 1.286 0.7 HATS-30b 1.175 0.706 HAT-P-30b 1.34 0.711 Kepler-49c 0.227 0.72 COROT-4b 1.19 0.72 WASP-35b 1.32 0.72 WASP-81b 1.429 0.729 K2-29b 1.19 0.73 TrES-1b 1.067 0.752 HAT-P-54b 0.944 0.76 HAT-P-33b 1.686 0.762 HATS-51b 1.41 0.768 HAT-P-29b 1.107 0.778 HAT-P-9b 1.4 0.78 HAT-P-66b 1.59 0.783 Kepler-23b 0.17 0.8 HAT-P-41b 1.685 0.8 WASP-92b 1.461 0.805 Lupus-TR-3b 0.89 0.81 Kepler-91b 1.367 0.81 NGTS-1b 1.33 0.812 HAT-P-52b 1.009 0.818 HATS-9b 1.065 0.837 COROT-9b 1.05 0.84 K2-115b 1.115 0.84 K2-107b 1.44 0.84 WASP-142b 1.53 0.84 Kepler-435b 1.99 0.84 COROT-29b 0.9 0.85 HATS-11b 1.51 0.85 HAT-P-13b 1.272 0.851 WASP-1b 1.483 0.854 WASP-16b 1.008 0.855 K2-238b 1.3 0.86 WASP-59b 0.775 0.863 KELT-8b 1.86 0.867 HATS-31b 1.64 0.88 WASP-23b 0.962 0.884 WASP-44b 1.14 0.889 WASP-58b 1.37 0.89 WASP-78b 1.7 0.89 HAT-P-45b 1.426 0.892 WASP-123b 1.318 0.899 WASP-79b 2.09 0.9 KELT-4Ab 1.699 0.902 WASP-28b 1.213 0.907 WASP-48b 1.396 0.907 KELT-15b 1.443 0.91 WASP-2b 1.071 0.915 COROT-12b 1.44 0.917 Kepler-54b
Load more

Recommended publications
  • Lurking in the Shadows: Wide-Separation Gas Giants As Tracers of Planet Formation
    Lurking in the Shadows: Wide-Separation Gas Giants as Tracers of Planet Formation Thesis by Marta Levesque Bryan In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy CALIFORNIA INSTITUTE OF TECHNOLOGY Pasadena, California 2018 Defended May 1, 2018 ii © 2018 Marta Levesque Bryan ORCID: [0000-0002-6076-5967] All rights reserved iii ACKNOWLEDGEMENTS First and foremost I would like to thank Heather Knutson, who I had the great privilege of working with as my thesis advisor. Her encouragement, guidance, and perspective helped me navigate many a challenging problem, and my conversations with her were a consistent source of positivity and learning throughout my time at Caltech. I leave graduate school a better scientist and person for having her as a role model. Heather fostered a wonderfully positive and supportive environment for her students, giving us the space to explore and grow - I could not have asked for a better advisor or research experience. I would also like to thank Konstantin Batygin for enthusiastic and illuminating discussions that always left me more excited to explore the result at hand. Thank you as well to Dimitri Mawet for providing both expertise and contagious optimism for some of my latest direct imaging endeavors. Thank you to the rest of my thesis committee, namely Geoff Blake, Evan Kirby, and Chuck Steidel for their support, helpful conversations, and insightful questions. I am grateful to have had the opportunity to collaborate with Brendan Bowler. His talk at Caltech my second year of graduate school introduced me to an unexpected population of massive wide-separation planetary-mass companions, and lead to a long-running collaboration from which several of my thesis projects were born.
    [Show full text]
  • Exoplanet Characterization with Nirspec
    Exoplanet Characterization with NIRSpec Jeff Valenti (STScI), Stephan Birkmann (ESA) Bernhard Dorner (MPIA) 1. Coupling optics 1 2. Fore optics 3. Filters 4. Focus 8 3 5. Apertures 6 4 6. Collimator 9 7. Gratings 7 5 2 8. Camera 9. Detectors 10. Lamps 10 1 NIRSpec Apertures Aperture Spectral Spatial S1600 1.6” 1.6” S400 0.4” 3.65” S200 0.2” 3.2” IFU 36 x 0.1” 3.6” MSA 2 x 95” 2 x 87” The S1600 aperture was designed for exoplanet observations 2 Noise Due to Jitter 1σ Jitter Jitter of 7 mas causes relative noise of 4 x 10-5 From PhD thesis Bernhard Dorner 3 NIRSpec Optical Configurations Grating Filter Wavelengths Resolution PRISM CLEAR 0.6 – 5.0 30 – 300 “100” F070LP 0.7 – 1.2 500 – 850 G140M F100LP 1.0 – 1.8 “1000” G235M F170LP 1.7 – 3.0 700 – 1300 G395M F290LP 2.9 – 5.0 F070LP 0.7 – 1.2 1300 – 2300 G140H F100LP 1.0 – 1.8 “2700” G235H F170LP 1.7 – 3.0 1900 – 3600 G395H F290LP 2.9 – 5.0 4 http://www.cosmos.esa.int/web/jwst/nirspec-performances 5 6 http://www.cosmos.esa.int/web/jwst/nirspec-performances Example of High-Resolution Model Spectra G395H Figure 4b of Burrows, Budaj, & Hubeny (2008) 7 Thermal Emission from a Hot Jupiter Adapted from Figure 4b of Burrows, Budaj, & Hubeny (2008) 8 Integrations and Exposures " An “exposure” is a sequence of integrations. " An “integration” is a sequence of groups, sampled up-the-ramp " One or more resets between integrations, but no other overheads " Currently using pixel-by-pixel resets, but row-by-row possible 9 Subarrays NX NY Frame time (s) Notes 2048 512 10.74 Full frame, 4 amps 2048 256 5.49
    [Show full text]
  • Extrasolar Planets
    Extrasolar Planets to appear in Encyclopedia of Time, Sage Publishing, in preparation, H.J. Birx (Ed.) The term extrasolar planets or exoplanets stands for planets outside our Solar System, i.e. not orbiting the Sun, but other stars. Planets in our Solar System are defined as objects with enough mass to be spherical and round by their own gravity and to be alone on their orbit around the Sun, i.e. to be the dominant object in a particular orbit, and not to be a moon or asteroid (see the entry Planet in this encyclopedia for the official definition, the historical debate, and a discussion of the planets of our Solar System). Most exoplanets are discovered by observing the stellar motion around the common center of mass of the star+planet system, i.e. by observing somehow the motion of the objects in orbit around each other, i.e. by measuring precisely the periodic variation of certain values, e.g. radial velocity or brightness, with time, e.g. the first extrasolar planets were found with the timing technique around a pulsating neutron star. The recent definition of Planets of our Solar System by the International Astronomical Union deals mainly with the question of the minimum mass for an object to qualify as planet and excludes Pluto. This matter was raised by the fact that more and more objects similar to Pluto were discovered by larger and larger telescopes. The questions of maximum mass and formation of planets were left out in this new definition, possibly partly because there is not yet a consensus in the international community.
    [Show full text]
  • The Slow Spin of the Young Sub-Stellar Companion GQ Lupi B and Its Orbital Configuration Henriette Schwarz1?, Christian Ginski1, Remco J
    Astronomy & Astrophysics manuscript no. AA-2016-28908-preprint c ESO 2016 July 4, 2016 The slow spin of the young sub-stellar companion GQ Lupi b and its orbital configuration Henriette Schwarz1?, Christian Ginski1, Remco J. de Kok1; 2, Ignas A. G. Snellen1, Matteo Brogi3; 5, and Jayne L. Birkby4; 6 1 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands 2 SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands 3 Center for Astrophysics and Space Astronomy, University of Colorado at Boulder, CO 80309 Boulder, USA 4 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MA 02138 Cambridge, USA 5 NASA Hubble Fellow 6 NASA Sagan Fellow ABSTRACT The spin of a planet or brown dwarf is related to the accretion process, and therefore studying spin can help promote our understand- ing of the formation of such objects. We present the projected rotational velocity of the young sub-stellar companion GQ Lupi b, along with its barycentric radial velocity. The directly imaged exoplanet or brown dwarf companion joins a small but growing en- semble of wide-orbit sub-stellar companions with a spin measurement. The GQ Lupi system was observed at high spectral resolution (R ∼100 000), and in the analysis we made use of both spectral and spatial filtering to separate the signal of the companion from that of the host star. We detect both CO (S/N=11.6) and H2O (S/N=7.7) in the atmosphere of GQ Lupi b by cross-correlating with model +0:9 −1 spectra, and we find it to be a slow rotator with a projected rotational velocity of 5:3−1:0 km s .
    [Show full text]
  • THE MASS of KOI-94D and a RELATION for PLANET RADIUS, MASS, and INCIDENT FLUX∗
    The Astrophysical Journal, 768:14 (19pp), 2013 May 1 doi:10.1088/0004-637X/768/1/14 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE MASS OF KOI-94d AND A RELATION FOR PLANET RADIUS, MASS, AND INCIDENT FLUX∗ Lauren M. Weiss1,12, Geoffrey W. Marcy1, Jason F. Rowe2, Andrew W. Howard3, Howard Isaacson1, Jonathan J. Fortney4, Neil Miller4, Brice-Olivier Demory5, Debra A. Fischer6, Elisabeth R. Adams7, Andrea K. Dupree7, Steve B. Howell2, Rea Kolbl1, John Asher Johnson8, Elliott P. Horch9, Mark E. Everett10, Daniel C. Fabrycky11, and Sara Seager5 1 B-20 Hearst Field Annex, Astronomy Department, University of California, Berkeley, Berkeley, CA 94720, USA; [email protected] 2 NASA Ames Research Center, Moffett Field, CA 94035, USA 3 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 4 Department of Astronomy & Astrophysics, University of California, Santa Cruz, 1156 High Street, 275 Interdisciplinary Sciences Building (ISB), Santa Cruz, CA 95064, USA 5 Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA 6 Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT 06510-8101, USA 7 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 8 California Institute of Technology, 1216 E. California Blvd., Pasadena, CA 91106, USA 9 Southern Connecticut State University, Department of Physics, 501 Crescent St., New Haven, CT 06515, USA 10 National Optical Astronomy Observatory, 950 N. Cherry Ave, Tucson, AZ 85719, USA 11 The Department of Astronomy and Astrophysics, University of Chicago, 5640 S.
    [Show full text]
  • The Search for Another Earth – Part II
    GENERAL ARTICLE The Search for Another Earth – Part II Sujan Sengupta In the first part, we discussed the various methods for the detection of planets outside the solar system known as the exoplanets. In this part, we will describe various kinds of exoplanets. The habitable planets discovered so far and the present status of our search for a habitable planet similar to the Earth will also be discussed. Sujan Sengupta is an 1. Introduction astrophysicist at Indian Institute of Astrophysics, Bengaluru. He works on the The first confirmed exoplanet around a solar type of star, 51 Pe- detection, characterisation 1 gasi b was discovered in 1995 using the radial velocity method. and habitability of extra-solar Subsequently, a large number of exoplanets were discovered by planets and extra-solar this method, and a few were discovered using transit and gravi- moons. tational lensing methods. Ground-based telescopes were used for these discoveries and the search region was confined to about 300 light-years from the Earth. On December 27, 2006, the European Space Agency launched 1The movement of the star a space telescope called CoRoT (Convection, Rotation and plan- towards the observer due to etary Transits) and on March 6, 2009, NASA launched another the gravitational effect of the space telescope called Kepler2 to hunt for exoplanets. Conse- planet. See Sujan Sengupta, The Search for Another Earth, quently, the search extended to about 3000 light-years. Both Resonance, Vol.21, No.7, these telescopes used the transit method in order to detect exo- pp.641–652, 2016. planets. Although Kepler’s field of view was only 105 square de- grees along the Cygnus arm of the Milky Way Galaxy, it detected a whooping 2326 exoplanets out of a total 3493 discovered till 2Kepler Telescope has a pri- date.
    [Show full text]
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • Temperate Earth-Sized Planets Transiting a Nearby Ultracool Dwarf Star
    1 Temperate Earth-sized planets transiting a nearby ultracool dwarf star Michaël Gillon1, Emmanuël Jehin1, Susan M. Lederer2, Laetitia Delrez1, Julien de Wit3, Artem Burdanov1, Valérie Van Grootel1, Adam J. Burgasser4, Amaury H. M. J. Triaud5, Cyrielle Opitom1, Brice-Olivier Demory6, Devendra K. Sahu7, Daniella Bardalez Gagliuffi4, Pierre Magain1 & Didier Queloz6 1Institut d’Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août 19C, 4000 Liège, Belgium. 2NASA Johnson Space Center, 2101 NASA Parkway, Houston, Texas, 77058, USA. 3Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, Massachusetts 02139, USA. 4Center for Astrophysics and Space Science, University of California San Diego, La Jolla, California 92093, USA. 5Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK. 6Astrophysics Group, Cavendish Laboratory, 19 J J Thomson Avenue, Cambridge, CB3 0HE, UK. 7Indian Institute of Astrophysics, Koramangala, Bangalore 560 034, India. Star-like objects with effective temperatures of less than 2,700 kelvin are referred to as ‘ultracool dwarfs'1. This heterogeneous group includes stars of extremely low mass as well as brown dwarfs (substellar objects not massive enough to sustain hydrogen fusion), and represents about 15 per cent of the population of astronomical objects near the Sun2. Core-accretion theory predicts that, given the small masses of these ultracool dwarfs, and the small sizes of their protoplanetary disk3,4, there should be a large but hitherto undetected population of terrestrial planets orbiting them5—ranging from metal-rich Mercury-sized planets6 to more hospitable volatile-rich Earth-sized planets7. Here we report observations of three short-period Earth-sized planets transiting an 2 ultracool dwarf star only 12 parsecs away.
    [Show full text]
  • Giant Planets
    Lyot Conference 5 June 2007 Properties of Exoplanets: from Giants toward Rocky Planets & Informing Coronagraphy Collaborators: Paul Butler, Debra Fischer, Steve Vogt Chris McCarthy, Jason Wright, John Johnson, Katie Peek Chris Tinney, Hugh Jones, Brad Carter Greg Laughlin, Doug Lin, Shigeru Ida, Jack Lissauer, Eugenio Rivera -Stellar Sample - 1330 Nearby FGKM Stars (~2000 stars total with Mayor et al. ) Star Selection Criteria: HipparcosH-R Cat. Diagram d < 100 pc . 1330 Target Stars •Vmag < 10 mag • No Close Binaries • Age > 2 Gyr Lum 1.3 Msun Target List: 0.3 M Published SUN 1 Michel Mayor & Didier Queloz First ExoPlanet 51 Peg Now Stephane Udry plays leadership role also. Doppler Monitering Begun: 1987 Uniform Doppler Precision: 1-3 m s-1 2000 FGKM M.S. Stars Three Telescopes 8 Years 7 Years 19 Years (3.5 AU) (3 AU) (6 AU) Keck Lick Anglo-Aus. Tel. 2 Precision: 1.5 m s-1 3 Years Planets or Brown Dwarfs in Unclosed, Long-Period Orbits: Targets for Coronagraphs 3 Sep ~ 0.3 “ Sep ~ 0.2 “ 4 Sep ~ 0.2” Examples of Jupiter-mass & Saturn mass Planets Detected by RV 5 Jupiter Mass Extrasolar Planets P = 5.3 yr e = 0.47 Jupiter Mass Extrasolar Planets P = 1.3 yr 6 Sub-Saturn Masses: 30 - 100 MEarth Msini = 32 MEarth Msini = 37 MEarth Msini = 57 MEarth Old Doppler Precision: 3 m/s Sub-Saturn Masses: Detectable for P < 2 Month Multiple - Planet Systems 7 HD 12661: Sun-like Star ) (meters/sec Velocity Time (years) 2 - Planet Model 2.5 M J Weak Interactions 1.9 MJ K0V, 1Gy, 16 pc HD 128311 2:1 Resonance Inner Outer Per (d) 458 918 Msini 2.3 3.1 ecc 0.23 0.22 ω 119 212 Pc / Pb = 2.004 Dynamical Resonance (Laughlin) 8 Msini = 1.4 MJ M Dwarfs have distant giant planets.
    [Show full text]
  • Exodata: a Python Package to Handle Large Exoplanet Catalogue Data
    ExoData: A Python package to handle large exoplanet catalogue data Ryan Varley Department of Physics & Astronomy, University College London 132 Hampstead Road, London, NW1 2PS, United Kingdom [email protected] Abstract Exoplanet science often involves using the system parameters of real exoplanets for tasks such as simulations, fitting routines, and target selection for proposals. Several exoplanet catalogues are already well established but often lack a version history and code friendly interfaces. Software that bridges the barrier between the catalogues and code enables users to improve the specific repeatability of results by facilitating the retrieval of exact system parameters used in an arti- cles results along with unifying the equations and software used. As exoplanet science moves towards large data, gone are the days where researchers can recall the current population from memory. An interface able to query the population now becomes invaluable for target selection and population analysis. ExoData is a Python interface and exploratory analysis tool for the Open Exoplanet Cata- logue. It allows the loading of exoplanet systems into Python as objects (Planet, Star, Binary etc) from which common orbital and system equations can be calculated and measured parame- ters retrieved. This allows researchers to use tested code of the common equations they require (with units) and provides a large science input catalogue of planets for easy plotting and use in research. Advanced querying of targets are possible using the database and Python programming language. ExoData is also able to parse spectral types and fill in missing parameters according to programmable specifications and equations. Examples of use cases are integration of equations into data reduction pipelines, selecting planets for observing proposals and as an input catalogue to large scale simulation and analysis of planets.
    [Show full text]
  • Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs
    Draft version July 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The California Legacy Survey I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades Lee J. Rosenthal,1 Benjamin J. Fulton,1, 2 Lea A. Hirsch,3 Howard T. Isaacson,4 Andrew W. Howard,1 Cayla M. Dedrick,5, 6 Ilya A. Sherstyuk,1 Sarah C. Blunt,1, 7 Erik A. Petigura,8 Heather A. Knutson,9 Aida Behmard,9, 7 Ashley Chontos,10, 7 Justin R. Crepp,11 Ian J. M. Crossfield,12 Paul A. Dalba,13, 14 Debra A. Fischer,15 Gregory W. Henry,16 Stephen R. Kane,13 Molly Kosiarek,17, 7 Geoffrey W. Marcy,1, 7 Ryan A. Rubenzahl,1, 7 Lauren M. Weiss,10 and Jason T. Wright18, 19, 20 1Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 2IPAC-NASA Exoplanet Science Institute, Pasadena, CA 91125, USA 3Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA 5Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 6Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 7NSF Graduate Research Fellow 8Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 9Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 10Institute for Astronomy, University of Hawai`i,
    [Show full text]
  • EPSC2018-126, 2018 European Planetary Science Congress 2018 Eeuropeapn Planetarsy Science Ccongress C Author(S) 2018
    EPSC Abstracts Vol. 12, EPSC2018-126, 2018 European Planetary Science Congress 2018 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2018 Stellar wind interaction with the expanding atmosphere of Gliese 436b A.G. Berezutskiy (1), I.F. Shaikhislamov (1), M.L. Khodachenko (2,3) and I.B. Miroshnichenko (1,4) (1) Institute of Laser Physics, Siberian Brunch Russian Academy of Science, Novosibirsk, Russia; (2) Space Research Institute, Austrian Academy of Science, Graz, Austria; (3) Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, Russia (4) Novosibirsk State Technical University, Novosibirsk, Russia ([email protected]) Abstract the escaping planetary upper atmospheric material are also taken into account. We study an exosphere of a Neptune-size exoplanet Gliese 436b, orbiting the red dwarf at an extremely 3. Results close distance (0.028 au), taking into account its interaction with the stellar wind plasma flow. It was At the initial state of the simulations, the atmosphere shown that Gliese 436 b has a bowshock region of Gliese 436b is assumed to consist of the molecular between planetary and stellar wind which localized hydrogen and helium atoms at a ratio NHe / NH2 = 1/5 on the distance of ~33 Rp, where density of planetary with the temperature 750 K. We consider the case of -3 atoms slightly dominates over the protons. a weak stellar wind (SW) with nsw=100 cm , Tsw=1 МК, Vsw=70 km/s, which is much less intense than 1. Introduction the solar wind. Because of this fact, , we did not consider generation of Energetic Neutral Atoms The modelled planet Gliese 436b has a mass (ENAs).
    [Show full text]