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{{Planetbox begin
Mcf
| name = TrES-2b
}}
{{Planetbox image
| image = TrES-2b.jpg
| caption = Artist's conception of TrES-2b, with unsubstantiated speculation on possible moons
}}
{{Planetbox star
| star = [[GSC 03549-02811]] A<ref name="binary" />
| constell = [[Draco (constellation)|Draco]]
| RA = {{RA|19|07|14.035}}
| DEC = {{DEC|+49|18|59.07}}
| dist_ly = {{val|750|30}}
| dist_pc = {{val|230|10}}
| class = G0V
}}
{{Planetbox orbit
| semimajor = {{val|0.03556|0.00075}}<ref name="binary" />
| eccentricity = 0
| period = {{val|2.47063|0.00001}}
| inclination = {{val|83.62|0.14}}<ref name="binary" />
| ang_dist = 0.167
}}
{{Planetbox character
| mass = {{val|1.199|0.052}}<ref name="binary" />
| radius = {{val|1.272|0.041}}<ref name="binary" />
| density =
| bond_albedo = 0.04
| geometric_albedo = 0.0136
| gravity_earth = {{val|3.284|0.016}}<ref name="binary" />
}}
{{Planetbox discovery
| discovery_date = August 21, 2006<br />confirmed September 8, 2006
| discoverers = O'Donovan et al.
| discovery_site = California & Arizona
| discovery_method = [[Transit method|Transit]]
| detection_methods = Radial velocity,<br>Reflection/emission modulations,<br>Ellipsoidal light variations,<br>Doppler beaming
| discovery_location = USA
| discovery_status=Published
}}
{{Planetbox catalog
| names=TrES-2b
}}
{{Planetbox reference
| star=TrES-2
| planet=
}}
{{Planetbox end}}
'''TrES-2b''' (or '''[[Kepler (spacecraft)|Kepler]]-1b''') is an [[extrasolar planet]] orbiting the [[star]] [[GSC 03549-02811]] located 750 [[light year]]s away from the [[Solar System]]. The planet has been identified in 2011 as the darkest known [[exoplanet]], reflecting less than 1% of any light that hits it.<ref name=darkest>{{cite journal | url=http://web.archive.org/web/20120317203801/http://www.astro.princeton.edu/~dsp/PrincetonSite/Home_files/darkest_world.pdf | author = David M. Kipping | author2 = David S. Spiegel | last-author-amp = yes | title = Detection of visible light from the darkest world | journal = [[Monthly Notices of the Royal Astronomical Society]] |accessdate=2011-08-12 | doi = 10.1111/j.1745-3933.2011.01127.x |arxiv = 1108.2297 |bibcode = 2011MNRAS.417L..88K }}</ref> The planet's mass and radius indicate that it is a [[gas giant]] with a bulk composition similar to that of [[Jupiter]]. Unlike Jupiter, but similar to many planets detected around other stars, TrES-2b is located very close to its star, and belongs to the class of planets known as [[hot Jupiter]]s. This system was within the [[field of view]] of the ''Kepler'' spacecraft.<ref name=disco>{{cite journal | url=http://www.iop.org/EJ/article/1538-4357/651/1/L61/21047.html | title=TrES-2: The First Transiting Planet in the Kepler Field | journal=[[The Astrophysical Journal]] Letters | volume=651 | date=2006 | pages=L61–L64 | doi=10.1086/509123 | bibcode=2006ApJ...651L..61O|arxiv = astro-ph/0609335 | issue=1 |last1=O'Donovan|first1=Francis T. | last2=Charbonneau | first2=David | last3=Mandushev | first3=Georgi | last4=Dunham | first4=Edward W. | last5=Latham | first5=David W. | last6=Torres | first6=Guillermo | last7=Sozzetti | first7=Alessandro | last8=Brown | first8=Timothy M. | last9=Trauger | first9=John T.| last10=Belmonte | first10=Juan A. | last11=Rabus | first11=Markus | last12=Almenara | first12=José M. | last13=Alonso | first13=Roi | last14=Deeg | first14=Hans J. | last15=Esquerdo | first15=Gilbert A. | last16=Falco | first16=Emilio E. | last17=Hillenbrand | first17=Lynne A. | last18=Roussanova | first18=Anna | last19=Stefanik | first19=Robert P. | last20=Winn | first20=Joshua N. | display-authors=8 }}</ref>

This planet continues to be studied by other projects and the parameters are being improved continuously. A 2007 study improved stellar and planetary parameters.<ref name="impro">{{ cite journal
| title=Improving Stellar and Planetary Parameters of Transiting Planet Systems: The Case of TrES-2
| journal=The Astrophysical Journal
| url=http://www.iop.org/EJ/article/0004-637X/664/2/1190/71636.html
| author=Alessandro Sozzetti
| date= August 1, 2007 | volume=664
| issue=2
| pages=1190–1198
| doi=10.1086/519214
| bibcode=2007ApJ...664.1190S|arxiv = 0704.2938 | last2=Torres
| first2=Guillermo
| last3=Charbonneau
| first3=David
| last4=Latham
| first4=David W.
| last5=Holman
| first5=Matthew J.
| last6=Winn
| first6=Joshua N.
| last7=Laird
| first7=John B.
| last8=o’Donovan
| first8=Francis T.
}}</ref> A 2008 study concluded that the TrES-2 system is a [[binary star]] system. This has a significant effect on the values for the stellar and the planetary parameters.<ref name=binary>{{cite journal
| url=http://www.mpia.de/homes/henning/Publications/daemgen.pdf
|format=PDF| title=Binarity of transit host stars&nbsp;— Implications for planetary parameters
| date=2009
| volume=498
| pages=567–574
| journal=[[Astronomy and Astrophysics]]
| doi=10.1051/0004-6361/200810988
| bibcode=2009A&A...498..567D
| last1=Daemgen
| first1=S.
| last2=Hormuth
| first2=F.
| last3=Brandner
| first3=W.
| last4=Bergfors
| first4=C.
| last5=Janson
| first5=M.
| last6=Hippler
| first6=S.
| last7=Henning
| first7=T.
| issue=2|arxiv = 0902.2179 }}</ref>

==Discovery==
[[Image:TrES-2 b rv.svg|thumb|left|The radial velocity of GSC 03549-02811 over time, caused by the presence of TrES-2 b.]]
TrES-2b was discovered on August 21, 2006 by the [[Trans-Atlantic Exoplanet Survey]] (TrES) by detecting the [[Transit method|transit]] of the planet across its parent star using Sleuth ([[Palomar Observatory]], [[California]]) and PSST ([[Lowell Observatory]], [[Arizona]]), part of the TrES network of 10–cm telescopes. The discovery was confirmed by the [[W. M. Keck Observatory]] on September 8, 2006, by measuring the radial velocity of the star that hosts TrES-2b.<ref name=disco />

==Spin-orbit angle==
In August 2008 more details of the relationship between the parent star and the orbit of the planet were published. The orbit was determined to be tilted by −{{val|9|12|s=°}} from the stellar equator. The orbital direction was determined to be in the same direction as the star's rotation (prograde).<ref>{{cite journal |url=http://www.iop.org/EJ/abstract/-search=62880448.10/0004-637X/682/2/1283|journal=The Astrophysical Journal |volume=682|pages= 1283–1288| doi=10.1086/589235| title= The Prograde Orbit of Exoplanet TrES-2b|date=2008 | bibcode=2008ApJ...682.1283W | issue=2| last1=Winn|first1=Joshua N. |last2=Johnson |first2=John Asher |last3=Narita |first3=Norio |last4=Suto |first4=Yasushi |last5=Turner |first5=Edwin L. |last6=Fischer |first6=Debra A. |last7=Butler |first7=R. Paul |last8=Vogt |first8=Steven S. |last9=O’Donovan |first9=Francis T.|last10=Gaudi |first10=B. Scott |arxiv = 0804.2259 |display-authors=8 }}</ref>

==The ''Kepler'' mission==
{{main|Kepler (spacecraft)}}
NASA launched ''Kepler'' in March 2009. The spacecraft is dedicated to the discovery of extrasolar planets by the [[transit method]] from [[solar orbit]]. In April 2009 the project released the [[First light (astronomy)|first light]] images from the spacecraft, and TrES-2b was one of two objects highlighted in these images. Although TrES-2b is not the only known exoplanet in the field of view of this spacecraft it is the only one identified in the first light images. This object is important for calibration and check-out.<ref name="kepler">{{cite web
| title=''Kepler'' Eyes Cluster and Known Planet
| url=http://www.nasa.gov/mission_pages/kepler/multimedia/images/fullFFIHot300.html
| publisher=NASA
| date=2009-04-16
| accessdate=2009-05-09}}</ref>
[[File:Kepler First Light Detail TrES-2.jpg|thumb|upright|The [[GSC 03549-02811]] system as seen from the [[Kepler (spacecraft)|''Kepler'' spacecraft]]. ([[Celestial coordinate system|Celestial north]] is toward the lower left corner and the subject is in the center of the photograph as seen clearly in enlarged view.)]]

Kepler mission also managed to detect the mass of the planet from Kepler data alone through the analysis of the light curve of the host star. In addition to detecting the planet directly, the planet was also detected by analysis of the star brightness caused by the gravitational tug of TrES-2b by shape distortion of the host star and by light variations due to Doppler beaming.<ref>[http://arxiv.org/abs/1210.4592 Photometrically derived masses and radii of the planet and star in the TrES-2 system]: Thomas Barclay, Daniel Huber, Jason F. Rowe, Jonathan J. Fortney, Caroline V. Morley, Elisa V. Quintana, Daniel C. Fabrycky, Geert Barentsen, Steven Bloemen, Jessie L. Christiansen, Brice-Olivier Demory, Benjamin J. Fulton, Jon M. Jenkins, Fergal Mullally, Darin Ragozzine, Shaun E. Seader, Avi Shporer, Peter Tenenbaum, Susan E. Thompson</ref>

===Darkest planet===
The first important result from the Kepler Mission about TrES-2b is an extremely low [[geometric albedo]], measured in 2011.<ref name=darkest/> If the entire day-night contrast were due to geometric albedo, it would be 2.53%, but modeling suggests that much of this is [[Black body|dayside emission]] and the true albedo is much lower. It is estimated to be less than 1% and for best-fit model it is about 0.04%. This makes TrES-2b the darkest known exoplanet, reflecting less light than coal or black acrylic paint.<ref name=darkest_news/> It is not clear why the planet is so dark. One reason could be an absence of reflective clouds such as those which make Jupiter so bright, due to TrES-2b's proximity to its parent star and the consequent high temperature. Another reason could be the presence in the atmosphere of light-absorbing chemicals such as vaporized sodium, potassium, or gaseous titanium oxide.<ref>{{cite web|url=http://www.astronomynow.com/news/n1108/11exo/|title=Exoplanet blacker than coal|last=Baldwin|first=Emily|work=Astronomy Now|date=2011-08-11|accessdate=2011-08-12}}</ref> In general, hot Jupiters are expected to be dark, because "absorption due to the broad wings of the sodium and potassium D lines is thought to dominate their visible spectra." Apart from that of [[Kepler-7b]] ({{val|38|12|s=%}}), albedo measurements for hot Jupiters have generally given only upper limits.<ref name=darkest/>

==References==
{{reflist|30em|refs=
<ref name=darkest_news>{{cite web
|url =http://www.space.com/12612-alien-planet-darkest-coal-black-kepler.html
|title =Coal-Black Alien Planet Is Darkest Ever Seen
|author =Charles Q. Choi
|publisher =Space.com
|date =2011-08-11
|accessdate =2014-12-26
|archiveurl =http://www.webcitation.org/68JlSDK2h
|archivedate=2012-06-10
|deadurl =no
}}</ref>
}}

==External links==
{{commons category|TrES-2 b|TrES-2b}}
*[http://www.nasa.gov/mission_pages/kepler/multimedia/images/TrES2Hot300.html Host to 'Hot Jupiter' (labeled)] NASA, 2009-04-16
* [http://www.astro.caltech.edu/~ftod/tres/tres2.html TrES-2: Most Massive Nearby Transiting Exoplanet]
* [http://pr.caltech.edu/media/Press_Releases/PR12890.html Jupiter-Sized Transiting Planet Found by Astronomers Using Novel Telescope Network]
* [http://www.perseus.gr/Astro-Photometry-TrES-2-20120529.htm Light curve for TrES-2b using differential photometry]
{{Sky|19|07|14|+|49|18|59|750}}

[[Category:Draco (constellation)]]
[[Category:Exoplanets discovered in 2006]]
[[Category:Exoplanets]]
[[Category:Giant planets]]
[[Category:Hot Jupiters]]
[[Category:Transiting exoplanets]]
[[Category:Exoplanets discovered by Kepler (spacecraft)]]

Revision as of 19:11, 8 February 2016

Template:Planetbox begin Template:Planetbox image Template:Planetbox star Template:Planetbox orbit Template:Planetbox character Template:Planetbox discovery Template:Planetbox catalog Template:Planetbox reference Template:Planetbox end TrES-2b (or Kepler-1b) is an extrasolar planet orbiting the star GSC 03549-02811 located 750 light years away from the Solar System. The planet has been identified in 2011 as the darkest known exoplanet, reflecting less than 1% of any light that hits it.[1] The planet's mass and radius indicate that it is a gas giant with a bulk composition similar to that of Jupiter. Unlike Jupiter, but similar to many planets detected around other stars, TrES-2b is located very close to its star, and belongs to the class of planets known as hot Jupiters. This system was within the field of view of the Kepler spacecraft.[2]

This planet continues to be studied by other projects and the parameters are being improved continuously. A 2007 study improved stellar and planetary parameters.[3] A 2008 study concluded that the TrES-2 system is a binary star system. This has a significant effect on the values for the stellar and the planetary parameters.[4]

Discovery

The radial velocity of GSC 03549-02811 over time, caused by the presence of TrES-2 b.

TrES-2b was discovered on August 21, 2006 by the Trans-Atlantic Exoplanet Survey (TrES) by detecting the transit of the planet across its parent star using Sleuth (Palomar Observatory, California) and PSST (Lowell Observatory, Arizona), part of the TrES network of 10–cm telescopes. The discovery was confirmed by the W. M. Keck Observatory on September 8, 2006, by measuring the radial velocity of the star that hosts TrES-2b.[2]

Spin-orbit angle

In August 2008 more details of the relationship between the parent star and the orbit of the planet were published. The orbit was determined to be tilted by −9±12° from the stellar equator. The orbital direction was determined to be in the same direction as the star's rotation (prograde).[5]

The Kepler mission

Main article: Kepler (spacecraft)

NASA launched Kepler in March 2009. The spacecraft is dedicated to the discovery of extrasolar planets by the transit method from solar orbit. In April 2009 the project released the first light images from the spacecraft, and TrES-2b was one of two objects highlighted in these images. Although TrES-2b is not the only known exoplanet in the field of view of this spacecraft it is the only one identified in the first light images. This object is important for calibration and check-out.[6]

The GSC 03549-02811 system as seen from the Kepler spacecraft. (Celestial north is toward the lower left corner and the subject is in the center of the photograph as seen clearly in enlarged view.)

Kepler mission also managed to detect the mass of the planet from Kepler data alone through the analysis of the light curve of the host star. In addition to detecting the planet directly, the planet was also detected by analysis of the star brightness caused by the gravitational tug of TrES-2b by shape distortion of the host star and by light variations due to Doppler beaming.[7]

Darkest planet

The first important result from the Kepler Mission about TrES-2b is an extremely low geometric albedo, measured in 2011.[1] If the entire day-night contrast were due to geometric albedo, it would be 2.53%, but modeling suggests that much of this is dayside emission and the true albedo is much lower. It is estimated to be less than 1% and for best-fit model it is about 0.04%. This makes TrES-2b the darkest known exoplanet, reflecting less light than coal or black acrylic paint.[8] It is not clear why the planet is so dark. One reason could be an absence of reflective clouds such as those which make Jupiter so bright, due to TrES-2b's proximity to its parent star and the consequent high temperature. Another reason could be the presence in the atmosphere of light-absorbing chemicals such as vaporized sodium, potassium, or gaseous titanium oxide.[9] In general, hot Jupiters are expected to be dark, because "absorption due to the broad wings of the sodium and potassium D lines is thought to dominate their visible spectra." Apart from that of Kepler-7b (38±12%), albedo measurements for hot Jupiters have generally given only upper limits.[1]

References

  1. ^ a b c David M. Kipping; David S. Spiegel. "Detection of visible light from the darkest world" (PDF). Monthly Notices of the Royal Astronomical Society. arXiv:1108.2297. Bibcode:2011MNRAS.417L..88K. doi:10.1111/j.1745-3933.2011.01127.x. Retrieved 2011-08-12. {{cite journal}}: Unknown parameter |last-author-amp= ignored (|name-list-style= suggested) (help)CS1 maint: unflagged free DOI (link)
  2. ^ a b O'Donovan, Francis T.; Charbonneau, David; Mandushev, Georgi; Dunham, Edward W.; Latham, David W.; Torres, Guillermo; Sozzetti, Alessandro; Brown, Timothy M.; et al. (2006). "TrES-2: The First Transiting Planet in the Kepler Field". The Astrophysical Journal Letters. 651 (1): L61–L64. arXiv:astro-ph/0609335. Bibcode:2006ApJ...651L..61O. doi:10.1086/509123.
  3. ^ Alessandro Sozzetti; Torres, Guillermo; Charbonneau, David; Latham, David W.; Holman, Matthew J.; Winn, Joshua N.; Laird, John B.; o’Donovan, Francis T. (August 1, 2007). "Improving Stellar and Planetary Parameters of Transiting Planet Systems: The Case of TrES-2". The Astrophysical Journal. 664 (2): 1190–1198. arXiv:0704.2938. Bibcode:2007ApJ...664.1190S. doi:10.1086/519214.
  4. ^ Daemgen, S.; Hormuth, F.; Brandner, W.; Bergfors, C.; Janson, M.; Hippler, S.; Henning, T. (2009). "Binarity of transit host stars — Implications for planetary parameters" (PDF). Astronomy and Astrophysics. 498 (2): 567–574. arXiv:0902.2179. Bibcode:2009A&A...498..567D. doi:10.1051/0004-6361/200810988.
  5. ^ Winn, Joshua N.; Johnson, John Asher; Narita, Norio; Suto, Yasushi; Turner, Edwin L.; Fischer, Debra A.; Butler, R. Paul; Vogt, Steven S.; et al. (2008). "The Prograde Orbit of Exoplanet TrES-2b". The Astrophysical Journal. 682 (2): 1283–1288. arXiv:0804.2259. Bibcode:2008ApJ...682.1283W. doi:10.1086/589235.
  6. ^ "Kepler Eyes Cluster and Known Planet". NASA. 2009-04-16. Retrieved 2009-05-09.
  7. ^ Photometrically derived masses and radii of the planet and star in the TrES-2 system: Thomas Barclay, Daniel Huber, Jason F. Rowe, Jonathan J. Fortney, Caroline V. Morley, Elisa V. Quintana, Daniel C. Fabrycky, Geert Barentsen, Steven Bloemen, Jessie L. Christiansen, Brice-Olivier Demory, Benjamin J. Fulton, Jon M. Jenkins, Fergal Mullally, Darin Ragozzine, Shaun E. Seader, Avi Shporer, Peter Tenenbaum, Susan E. Thompson
  8. ^ Charles Q. Choi (2011-08-11). "Coal-Black Alien Planet Is Darkest Ever Seen". Space.com. Archived from the original on 2012-06-10. Retrieved 2014-12-26. {{cite web}}: Unknown parameter |deadurl= ignored (|url-status= suggested) (help)
  9. ^ Baldwin, Emily (2011-08-11). "Exoplanet blacker than coal". Astronomy Now. Retrieved 2011-08-12.
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