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'''HD 15082''' (also known as '''WASP-33''') is a [[star]] located roughly 399 [[light year]]s away<ref name="Gaia DR2"/> in the northern constellation of [[Andromeda (constellation)|Andromeda]].<ref>{{cite web|url=http://var2.astro.cz/ETD/etd.php?STARNAME=WASP-33&PLANET=b|title=WASP-33 b|work=ETD - Exoplanet Transit Database|accessdate=2010-04-28}}</ref> The star is a [[Delta Scuti variable]]<ref name=Essen2014/> and a planetary transit variable. A [[hot Jupiter]] type [[extrasolar planet]], '''HD 15082b''' or '''WASP-33b''', orbits this star with an orbital period of 1.22&nbsp;days. It is the first Delta Scuti variable known to host a planet.<ref name=sd20110119/>
'''HD 15082''' (also known as '''WASP-33''') is a [[star]] located roughly 399 [[light year]]s away<ref name="Gaia DR2"/> in the northern constellation of [[Andromeda (constellation)|Andromeda]].<ref>{{cite web|url=http://var2.astro.cz/ETD/etd.php?STARNAME=WASP-33&PLANET=b|title=WASP-33 b|work=ETD - Exoplanet Transit Database|accessdate=2010-04-28}}</ref> The star is a [[Delta Scuti variable]]<ref name=Essen2014/> and a planetary transit variable. A [[hot Jupiter]] type [[extrasolar planet]], named [[WASP-33b]] or '''HD 15082b''', orbits this star with an orbital period of 1.22&nbsp;days. It is the first Delta Scuti variable known to host a planet.<ref name=sd20110119/>


==Spectrum==
==Spectrum==
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==Pulsations==
==Pulsations==
Delta Scuti variables usually exhibit many [[Asteroseismology|pulsation modes]], and HD 15082 is no exception, with 8 measured high frequency p-modes<ref name=Essen2014/>. Another proposed non-radial mode, which could be induced by tidal interactions with the planet, would make this star also a [[Gamma Doradus variables]].<ref name="cameron2010"/>
Delta Scuti variables usually exhibit many [[Asteroseismology|pulsation modes]], and HD 15082 is no exception, with 8 measured high frequency p-modes<ref name=Essen2014/>. Another proposed non-radial mode, which could be induced by tidal interactions with the planet, would make this star also a [[Gamma Doradus variable]].<ref name="cameron2010"/>


==Planet==
==Planet==
In 2010, the [[SuperWASP]] project announced the discovery of an [[extrasolar planet]], designated '''HD 15082 b''', orbiting the star. The discovery was made by detecting the [[transit (astronomy)|transit]] of the planet as it passes in front of its star, an event which occurs every 1.22&nbsp;days.

{{OrbitboxPlanet begin|table_ref=<ref name="cameron2010" /><ref name="Zhang2017"/><ref group="note">Parameters from the photometric + radial velocity solution in table 3 of Cameron ''et al.'' (2010). Different analysis methods result in slightly different parameters, see Cameron ''et al.'' (2010) for details.</ref>}}
{{OrbitboxPlanet begin|table_ref=<ref name="cameron2010" /><ref name="Zhang2017"/><ref group="note">Parameters from the photometric + radial velocity solution in table 3 of Cameron ''et al.'' (2010). Different analysis methods result in slightly different parameters, see Cameron ''et al.'' (2010) for details.</ref>}}
{{OrbitboxPlanet
{{OrbitboxPlanet
| exoplanet = b
| exoplanet = [[WASP-33b|b]]
| mass = < 4.59
| mass = < 4.59
| period = {{nowrap|{{val|1.21987089}} ± {{val|1.5|e=-07}}}}
| period = {{nowrap|{{val|1.21987089}} ± {{val|1.5|e=-07}}}}
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}}
}}
{{Orbitbox end}}
{{Orbitbox end}}
In 2010, the [[SuperWASP]] project announced the discovery of an [[extrasolar planet]], designated '''HD 15082 b''', orbiting the star. The discovery was made by detecting the [[transit (astronomy)|transit]] of the planet as it passes in front of its star, an event which occurs every 1.22&nbsp;days. As the planet crosses the star's disc, it causes the rotational broadening signature in the star's spectrum to change, enabling the determination of the sky-projected angle between the star's equator and the orbital plane of the planet to be determined. (This differs from the [[Rossiter–McLaughlin effect]] which is observed for radial velocity measurements). For HD 15082 b, this angle is about 250&nbsp;degrees, indicating that it is in a retrograde orbit. Limits from radial velocity measurements imply it has less than 4.1 times the mass of Jupiter.<ref name="cameron2010" /> The [[exoplanet]] orbits so close to its star that its surface temperature is about {{Convert|3200|°C|°F}}.<ref>{{Cite web|title = Hottest planet is hotter than some stars|url = https://www.newscientist.com/article/dn19991-hottest-planet-is-hotter-than-some-stars.html#.VXqvYc9Viko|accessdate = 2015-06-12}}</ref>. The transit was later recovered in [[Hipparcos]] data.<ref name=McDonald2018/>

June 2015 NASA reported the exoplanet has a [[stratosphere]], and the [[atmosphere]] contains [[titanium oxide]] which creates the stratosphere. Titanium oxide is one of only a few compounds that is a strong absorber of visible and ultraviolet radiation, which heats the atmosphere, and able to exist in a gas-state in a hot atmosphere.<ref name="NASA-20150611">{{Cite web|title = NASA's Hubble Telescope Detects 'Sunscreen' Layer on Distant Planet|url = http://www.nasa.gov/press-release/nasa-s-hubble-telescope-detects-sunscreen-layer-on-distant-planet|accessdate = 2015-06-11|date = 2015-06-11}}</ref><ref>{{cite journal |title = Spectroscopic Evidence for a Temperature Inversion in the Dayside Atmosphere of the Hot Jupiter WASP-33b|journal= The Astrophysical Journal|volume= 806|issue= 2|pages= 146|arxiv= 1505.01490|first = Korey|last = Haynes|first2 = Avi M.|last2 = Mandell|first3 = Nikku|last3 = Madhusudhan|first4 = Drake|last4 = Deming|first5 = Heather|last5 = Knutson|bibcode = 2015ApJ...806..146H |doi = 10.1088/0004-637X/806/2/146 |year= 2015}}</ref>
{{Clear}}
[[File:15-121a-HubbleDetectsStratosphereOnWASP33b-20150611.jpg|thumb|300px|center|<center>Atmosphere of WASP-33b was detected by monitoring light as the planet passed behind its star (top) - Higher temperatures result in the low stratosphere due to molecules absorbing radiation from the star (right) - Lower temperatures at higher altitudes would result if there were no stratosphere (left).<ref name="NASA-20150611" /></center>]]

===Non-Keplerian features of motion for HD 15082 b===
In view of the high rotational speed of its parent star, the orbital motion of HD 15082 b may be affected in a measurable way by the huge [[oblateness]] of the star and effects of general relativity.

First, the distorted shape of the star makes its [[gravitational field]] deviate from the usual [[Newtonian mechanics|Newtonian]] inverse-square law. The same is true for the Sun, and part of the [[Tests of general relativity#Perihelion precession of Mercury|precession of the orbit of Mercury]] is due to this effect. However, it is estimated to be <math>9 \times 10^9</math> greater for HD 15082b.<ref name = "iorio2006" />

Other effects will also be greater for HD 15082b. In particular, [[precession]] due to general relativistic [[frame-dragging]] should be <math>3 \times 10^5</math> greater for HD 15082b than for Mercury, where it is so far too small to have been observed. It has been argued that the oblateness of HD 15082 could be measured at a percent accuracy from a 10-year analysis of the time variations of the planet's transits.<ref name = "iorio2006" /> Effects due to the planet's oblateness are smaller by at least one order of magnitude, and they depend on the unknown angle between the planet’s equator and the orbital plane, perhaps making them undetectable. The effects of frame-dragging are slightly too small to be measured by such an experiment.


==See also==
==See also==
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<ref name="Gaia DR2">{{Cite Gaia DR2|328636019723252096}}</ref>
<ref name="Gaia DR2">{{Cite Gaia DR2|328636019723252096}}</ref>

<ref name="iorio2006">{{citation|title = Classical and relativistic node precessional effects in WASP-33b and perspectives for detecting them|journal = Astrophysics and Space Science|arxiv = 1006.2707 |date = 2010-07-25|first = Lorenzo|last = Iorio|doi = 10.1007/s10509-010-0468-x |bibcode = 2011Ap&SS.331..485I |volume=331 |issue = 2|pages=485–496}}</ref>


<ref name=sd20110119>{{citation | work=Science Daily | url=http://www.spacedaily.com/reports/Discovery_Of_A_Pulsating_Star_That_Hosts_A_Giant_Planet_999.html | title=Discovery Of A Pulsating Star That Hosts A Giant Planet | date=January 19, 2011 }}</ref>
<ref name=sd20110119>{{citation | work=Science Daily | url=http://www.spacedaily.com/reports/Discovery_Of_A_Pulsating_Star_That_Hosts_A_Giant_Planet_999.html | title=Discovery Of A Pulsating Star That Hosts A Giant Planet | date=January 19, 2011 }}</ref>
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| volume=355 | pages=L27–L30 | year=2000
| volume=355 | pages=L27–L30 | year=2000
| bibcode=2000A&A...355L..27H | postscript=. }}</ref>
| bibcode=2000A&A...355L..27H | postscript=. }}</ref>

<ref name=McDonald2018>{{cite journal|bibcode=2018MNRAS.477L..21M|title=Pre-discovery transits of the exoplanets WASP-18b and WASP-33b from Hipparcos|journal=Monthly Notices of the Royal Astronomical Society|volume=477|issue=1|pages=L21|last1=McDonald|first1=I.|last2=Kerins|first2=E.|year=2018}}</ref>


<ref name=Goyal2018>{{cite journal|bibcode=2018MNRAS.474.5158G|title=A library of ATMO forward model transmission spectra for hot Jupiter exoplanets|journal=Monthly Notices of the Royal Astronomical Society|volume=474|issue=4|pages=5158|last1=Goyal|first1=Jayesh M.|last2=Mayne|first2=Nathan|last3=Sing|first3=David K.|last4=Drummond|first4=Benjamin|last5=Tremblin|first5=Pascal|last6=Amundsen|first6=David S.|last7=Evans|first7=Thomas|last8=Carter|first8=Aarynn L.|last9=Spake|first9=Jessica|last10=Baraffe|first10=Isabelle|last11=Nikolov|first11=Nikolay|last12=Manners|first12=James|last13=Chabrier|first13=Gilles|last14=Hebrard|first14=Eric|year=2018}}</ref>
<ref name=Goyal2018>{{cite journal|bibcode=2018MNRAS.474.5158G|title=A library of ATMO forward model transmission spectra for hot Jupiter exoplanets|journal=Monthly Notices of the Royal Astronomical Society|volume=474|issue=4|pages=5158|last1=Goyal|first1=Jayesh M.|last2=Mayne|first2=Nathan|last3=Sing|first3=David K.|last4=Drummond|first4=Benjamin|last5=Tremblin|first5=Pascal|last6=Amundsen|first6=David S.|last7=Evans|first7=Thomas|last8=Carter|first8=Aarynn L.|last9=Spake|first9=Jessica|last10=Baraffe|first10=Isabelle|last11=Nikolov|first11=Nikolay|last12=Manners|first12=James|last13=Chabrier|first13=Gilles|last14=Hebrard|first14=Eric|year=2018}}</ref>

Revision as of 18:00, 24 January 2019

HD 15082
Observation data
Epoch J2000      Equinox J2000
Constellation Andromeda
Right ascension 02h 26m 51.0583s[1]
Declination +37° 33′ 01.7377″[1]
Apparent magnitude (V) 8.3[2]
Characteristics
Spectral type kA5hA8mF4[3]
B−V color index 0.27[4]
Variable type δ Sct[2]
Astrometry
Radial velocity (Rv)−9.20±2.8[5] km/s
Proper motion (μ) RA: −0.976±0.118[1] mas/yr
Dec.: −8.977±0.105[1] mas/yr
Parallax (π)8.1724 ± 0.0661 mas[1]
Distance399 ± 3 ly
(122.4 ± 1.0 pc)
Details
Mass1.55 ± 0.04[3] M☉
Radius1.51[6] R☉
Surface gravity (log g)4.3 ± 0.2[2] cgs
Temperature7,400 ± 200[2] K
Metallicity [Fe/H]0.1 ± 0.2[3] dex
Rotational velocity (v sin i)86[2] km/s
Age100[7] Myr
Other designations
BD+36 489, HD 15082, HIP 11397, SAO 55561, WASP-33.
Database references
SIMBADdata

HD 15082 (also known as WASP-33) is a star located roughly 399 light years away[1] in the northern constellation of Andromeda.[8] The star is a Delta Scuti variable[9] and a planetary transit variable. A hot Jupiter type extrasolar planet, named WASP-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.[10]

Spectrum

HD 15082 is an Am star, which makes its stellar classification challenging to discern. The hydrogen lines and effective temperature of the star are similar to spectral type A8, however the calcium II K line resembles that of an A5 star, and the metallic lines are more similar to an F4 star. The spectral type is thus written kA5hA8mF4.[3]

Pulsations

Delta Scuti variables usually exhibit many pulsation modes, and HD 15082 is no exception, with 8 measured high frequency p-modes[9]. Another proposed non-radial mode, which could be induced by tidal interactions with the planet, would make this star also a Gamma Doradus variable.[3]

Planet

In 2010, the SuperWASP project announced the discovery of an extrasolar planet, designated HD 15082 b, orbiting the star. The discovery was made by detecting the transit of the planet as it passes in front of its star, an event which occurs every 1.22 days.

The HD 15082 planetary system[3][11][note 1]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b < 4.59 MJ 0.02558 (± 0.00023) 1.21987089 ± 1.5×10−07 0 87.67° 1.438 RJ

See also

Notes

  1. ^ Parameters from the photometric + radial velocity solution in table 3 of Cameron et al. (2010). Different analysis methods result in slightly different parameters, see Cameron et al. (2010) for details.

References

  1. ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ a b c d e Herrero, E.; et al. (February 2011), "WASP-33: the first δ Scuti exoplanet host star" (PDF), Astronomy and Astrophysics, 526: L10, arXiv:1010.1173, Bibcode:2011A&A...526L..10H, doi:10.1051/0004-6361/201015875
  3. ^ a b c d e f 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.
  4. ^ 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.
  5. ^ Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv:1606.08053, Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065.
  6. ^ 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. Bibcode:2018MNRAS.474.5158G.
  7. ^ 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
  8. ^ "WASP-33 b". ETD - Exoplanet Transit Database. Retrieved 2010-04-28.
  9. ^ 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.
  10. ^ "Discovery Of A Pulsating Star That Hosts A Giant Planet", Science Daily, January 19, 2011
  11. ^ 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. doi:10.3847/1538-3881/aaa458.{{cite journal}}: CS1 maint: unflagged free DOI (link)
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