Star in the constellation Andromeda
HD 15082 A
light curve for V807 Andromedae (HD 15082), plotted from
TESS data.
[ 1] The deep minima are caused by the planet transits.
Observation dataEpoch J2000 Equinox J2000 Constellation Andromeda [ 2] Right ascension 02h 26m 51.0583s [ 3] Declination +37° 33′ 01.736″[ 3] Apparent magnitude (V)8.3[ 4] Characteristics Evolutionary stage main sequence [ 3] Spectral type kA5hA8mF4[ 5] B−Vcolor index 0.27[ 6] Variable type δ Sct [ 4] planetary transit Astrometry Radial velocity (Rv )± 0.33[ 3] km/s Proper motion (μ)RA: mas /yr [ 3] Dec.: mas /yr [ 3] Parallax (π)8.2238± 0.0327 mas [ 3] Distance 397 ± 2 ly pc ) Absolute magnitude (MV )+2.85[ 2] Details Mass ± 0.031[ 7] M ☉ Radius ± 0.034[ 7] R ☉ Luminosity 6.6[ 3] L ☉ Surface gravity (log g )4.3± 0.2[ 4] cgs Temperature ± 100[ 7] K Metallicity [Fe/H] 0.1± 0.2[ 8] dex Rotational velocity (v sin i )86[ 4] Age 100[ 9] Myr Other designations V807 And ,BD +36 489HD 15082HIP 11397SAO 55561TOI -1599TIC 129979528WASP -332MASS J02265106+3733017[ 10] Database references SIMBAD data Exoplanet Archive data
HD 15082 (also known asWASP-33 ) is astar located 397light years away[ 3] Andromeda .[ 11] Delta Scuti variable [ 12] hot Jupiter typeextrasolar planet , namedWASP-33b or HD 15082b, orbits this star with an orbital period of 1.22 days. It is the first Delta Scuti variable known to host a planet.[ 13]
HD 15082 is anAm star , which makes itsstellar classification challenging to discern. Thehydrogen lines andeffective temperature of the star are similar to spectral type A8, however thecalcium II K line resembles that of an A5 star, and the metallic lines are more similar to an F4 star. The spectral type is written kA5hA8mF4.[ 8] [ 9] projected rotational velocity of 86 km/s.[ 4] [ 8] [ 14]
The intrinsic variability of HD 15082 was discovered in 2011 by Enrique Herreroet al. [ 4] pulsation modes , and HD 15082 is no exception, with 8 measured high frequency p-modes.[ 12] Gamma Doradus variable .[ 8] variable star designation V807 Andromedae .[ 15]
In 2010, theSuperWASP project announced the discovery of anexoplanet , designatedWASP-33b , orbiting the star. The discovery was made by detecting thetransit of the planet as it passes in front of its star, an event which occurs every 1.22 days.[ 8] [ 16]
^ "MAST: Barbara A. Mikulski Archive for Space Telescopes" . Space Telescope Science Institute. Retrieved8 December 2021 .^a b Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation".Astronomy Letters .38 (5): 331.arXiv :1108.4971 Bibcode :2012AstL...38..331A .doi :10.1134/S1063773712050015 . ^a b c d e f g h Vallenari, A.; et al. (Gaia collaboration) (2023)."Gaia Data Release 3. Summary of the content and survey properties" .Astronomy and Astrophysics .674 : A1.arXiv :2208.00211 Bibcode :2023A&A...674A...1G .doi :10.1051/0004-6361/202243940 S2CID 244398875 . Gaia DR3 record for this source atVizieR .^a b c d e f Herrero, E.; et al. (February 2011). "WASP-33: the first δ Scuti exoplanet host star".Astronomy and Astrophysics .526 : L10.arXiv :1010.1173 Bibcode :2011A&A...526L..10H .doi :10.1051/0004-6361/201015875 .S2CID 37446555 . ^ Grenier, S.; Baylac, M. -O.; Rolland, L.; Burnage, R.; Arenou, F.; Briot, D.; Delmas, F.; Duflot, M.; Genty, V.; Gómez, A. E.; Halbwachs, J. -L.; Marouard, M.; Oblak, E.; Sellier, A. (1999). "Radial velocities. Measurements of 2800 B2-F5 stars for HIPPARCOS".Astronomy and Astrophysics Supplement Series .137 : 451.Bibcode :1999A&AS..137..451G .doi :10.1051/aas:1999489 . ^ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars".Astronomy & Astrophysics .355 :L27 – L30 .Bibcode :2000A&A...355L..27H . ^a b c d Chakrabarty, Aritra; Sengupta, Sujan (July 2019)."Precise Photometric Transit Follow-up Observations of Five Close-in Exoplanets: Update on Their Physical Properties" .The Astronomical Journal 158 (1): 39.arXiv :1905.11258 Bibcode :2019AJ....158...39C .doi :10.3847/1538-3881/ab24dd ^a b c d e Collier Cameron, A.; et al. (2010)."Line-profile tomography of exoplanet transits - II. A gas-giant planet transiting a rapidly rotating A5 star" .Monthly Notices of the Royal Astronomical Society 407 (1): 507.arXiv :1004.4551 Bibcode :2010MNRAS.407..507C .doi :10.1111/j.1365-2966.2010.16922.x S2CID 11989684 . ^a b Moya, A.; et al. (November 2011). "High spatial resolution imaging of the star with a transiting planet WASP-33".Astronomy & Astrophysics .535 : A110.arXiv :1110.3160 Bibcode :2011A&A...535A.110M .doi :10.1051/0004-6361/201116889 .S2CID 54591538 . ^ "HD 15082" .SIMBAD Centre de données astronomiques de Strasbourg .^ "WASP-33 b" .ETD - Exoplanet Transit Database . Retrieved2010-04-28 .^a b von Essen, C.; Czesla, S.; Wolter, U.; Breger, M.; Herrero, E.; Mallonn, M.; Ribas, I.; Strassmeier, K. G.; Morales, J. C. (2014). "Pulsation analysis and its impact on primary transit modeling in WASP-33".Astronomy and Astrophysics .561 : A48.arXiv :1311.3614 Bibcode :2014A&A...561A..48V .doi :10.1051/0004-6361/201322453 .S2CID 119213599 . ^ "Discovery Of A Pulsating Star That Hosts A Giant Planet" .Science Daily . January 19, 2011.^ Goyal, Jayesh M.; Mayne, Nathan; Sing, David K.; Drummond, Benjamin; Tremblin, Pascal; Amundsen, David S.; Evans, Thomas; Carter, Aarynn L.; Spake, Jessica; Baraffe, Isabelle; Nikolov, Nikolay; Manners, James; Chabrier, Gilles; Hebrard, Eric (2018)."A library of ATMO forward model transmission spectra for hot Jupiter exoplanets" .Monthly Notices of the Royal Astronomical Society .474 (4): 5158.arXiv :1710.10269 Bibcode :2018MNRAS.474.5158G .doi :10.1093/mnras/stx3015 hdl :10871/30324 S2CID 55105931 . ^ "GCVS Query forms" .^ Christian, D. J.; Pollacco, D. L.; Skillen, I.; Street, R. A.; Keenan, F. P.; Clarkson, W. I.; Collier Cameron, A.; Kane, S. R.; Lister, T. A.; West, R. G.; Enoch, B.; Evans, A.; Fitzsimmons, A.; Haswell, C. A.; Hellier, C.; Hodgkin, S. T.; Horne, K.; Irwin, J.; Norton, A. J.; Osborne, J. (November 2006)."The SuperWASP wide-field exoplanetary transit survey: candidates from fields 23 h < RA < 03 h" .Monthly Notices of the Royal Astronomical Society .372 (3):1117– 1128.Bibcode :2006MNRAS.372.1117C .doi :10.1111/j.1365-2966.2006.10913.x hdl :10211.3/172060 . Retrieved10 November 2024 . ^ Zhang, Michael; et al. (2017)."Phase curves of WASP-33b and HD 149026b and a New Correlation Between Phase Curve Offset and Irradiation Temperature" .The Astronomical Journal .155 (2): 83.arXiv :1710.07642 Bibcode :2018AJ....155...83Z .doi :10.3847/1538-3881/aaa458 S2CID 54755276 .
