HR 8799 c

HR 8799 c
Exoplanet List of exoplanets

Size comparison of HR 8799 c (gray) with Jupiter.
Parent star
Star HR 8799
Constellation Pegasus
Right ascension (α) 23h 07m 28.7150s[1]
Declination (δ) +21° 08′ 03.302″[1]
Apparent magnitude (mV) 5.964[1]
Distance129 ± 4[2][note 1] ly
(39 ± 1[2][note 1] pc)
Spectral type kA5 hF0 mA5 V; λ Boo[3][4]
Observed separation
Observation epoch 2008-09-18
Angular separation (ρ) 964[5][note 2] mas
Position angle (θ) 317.06[5][note 2]°
Projected separation (d) 38[5] AU
Orbital elements
Semi-major axis(a) ~ 38[5][note 3] AU
(~ 5600 Gm)
Orbital period(P) ~ 190[5][note 3] y
Physical characteristics
Mass(m)7+3
−2[6] MJ
Radius(r)1.3[7] RJ
Density(ρ)3.2+1.3
−0.7 kg m−3
Temperature (T) 1090+10
−90[5]
Discovery information
Discovery date November 13, 2008
Discoverer(s) Marois et al.
Discovery method Direct imaging
Discovery site Keck and Gemini
observatories in Hawaii
Discovery status Published
Other designations
HD 218396 c[8]
Database references
Extrasolar Planets
Encyclopaedia		data
SIMBADdata
Exoplanet Archivedata
Open Exoplanet Cataloguedata

HR 8799 c is an extrasolar planet located approximately 129 light-years away in the constellation of Pegasus, orbiting the 6th magnitude Lambda Boötis star HR 8799. This planet has a mass between 5 and 10 Jupiter masses and a radius from 20 to 30% larger than Jupiter's. It orbits at 38 AU from HR 8799 with an unknown eccentricity and a period of 190 years; it is the 2nd planet discovered in the HR 8799 system. Along with two other planets orbiting HR 8799, this planet was discovered on November 13, 2008 by Marois et al., using the Keck and the Gemini observatories in Hawaii. These planets were discovered using the direct imaging technique.[5][9][10][11][12] In January 2010, HR 8799 c became the 3rd exoplanet to have a portion of its spectrum directly observed (following 2M1207b and 1RXS J1609b), confirming the feasibility of direct spectrographic studies of exoplanets.[7][13]

Spectra

Spectrum of planet around HR8799. Credit: ESO/M. Janson.
The spectrum of the planet HR 8799 c. The spectrum of the star and the planet was obtained with the NACO adaptive optics instrument on ESO’s Very Large Telescope.

Near infrared spectroscopy from 995 to 1769 nanometers made with the Palomar Observatory show evidence of Ammonia, perhaps some Acetylene but neither Carbon Dioxide nor substantial Methane.[14] High resolution spectroscopy with the OSIRIS instrument on the Keck Observatory show numerous well resolved lines of molecular absorption in the planet's atmosphere in the K band. Although methane is absent, the planet's atmosphere contains both water and carbon monoxide; the carbon-to-oxygen ratio of HR 8799 c is higher than that of its star, suggesting that the planet formed through the core accretion process.[15][16]

See also

Notes

  1. 1 2 Computed from parallax: \scriptstyle \mathrm{distance\ in\ parsecs}=\frac{1000}{\mathrm{parallax\ in\ milliarcseconds}}
  2. 1 2 Calculated from the separations in the East and North directions which are −0.657 and 0.706 arcseconds respectively.
  3. 1 2 Value given assuming the planet's orbit is circular and is being observed face-on.

References

  1. 1 2 3 V* V342 Peg -- Variable Star of gamma Dor type, entry, SIMBAD. Accessed on line November 14, 2008.
  2. 1 2 van Leeuwen, F. (2007). "HIP 114189". Hipparcos, the New Reduction. Retrieved 2008-10-13.
  3. ↑ Gray, R.O. and Kaye, A.B. (1999). "HR 8799: A Link between γ Doradus Variables and λ Bootis Stars". The Astronomical Journal 118 (6): 2993–2996. Bibcode:1999AJ....118.2993G. doi:10.1086/301134.
  4. ↑ Kaye, A.B.; et al. (1999). "Gamma Doradus Stars: Defining a New Class of Pulsating Variables". PASP 111 (761): 840–844. arXiv:astro-ph/9905042. Bibcode:1999PASP..111..840K. doi:10.1086/316399.
  5. 1 2 3 4 5 6 7 Marois, Christian; et al. (November 2008). "Direct Imaging of Multiple Planets Orbiting the Star HR 8799". Science 322 (5906): 1348–1352. arXiv:0811.2606. Bibcode:2008Sci...322.1348M. doi:10.1126/science.1166585. PMID 19008415.
  6. ↑ Marois; Zuckerman; Konopacky; Macintosh; Barman (2010). "Images of a fourth planet orbiting HR 8799". arXiv:1011.4918 [astro-ph.EP].
  7. 1 2 Jason, M.; C. Bergfors; M. Goto; W. Brandner; D. Lafrenière (2010). "Spatially resolved spectroscopy of the exoplanet HR 8799 c" (PDF). The Astrophysical Journal. arXiv:1001.2017. Bibcode:2010ApJ...710L..35J. doi:10.1088/2041-8205/710/1/l35. Retrieved 2010-01-13.
  8. ↑ HD 218396c -- Extra-solar Planet Candidate, entry, SIMBAD. Accessed on line December 6, 2008.
  9. ↑ "Astronomers capture first images of newly-discovered solar system" (Press release). W. M. Keck Observatory. 2008-11-13. Retrieved 2008-12-02.
  10. ↑ "Gemini Releases Historic Discovery Image of Planetary First Family" (Press release). Gemini Observatory. 2008-11-13. Retrieved 2008-12-02.
  11. ↑ Achenbach, Joel (2008-11-13). "Scientists Publish First Direct Images of Extrasolar Planets". The Washington Post (The Washington Post Company). Retrieved 2008-12-02.
  12. ↑ Fabrycky; et al. (1 December 2008). "Stability of the directly imaged multiplanet system HR 8799: resonance and masses". Astrophys. J. 710 (2): 1408–1421. arXiv:0812.0011. Bibcode:2010ApJ...710.1408F. doi:10.1088/0004-637X/710/2/1408.
  13. ↑ Janson, M. (13 January 2010). "VLT Captures First Direct Spectrum of an Exoplanet". ESO (La Silla Observatory). Retrieved 2010-01-13.
  14. ↑ B. R. Oppenheimer. "Reconnaissance of the HR 8799 Exosolar System I: Near IR Spectroscopy". Cornell University. arXiv:1303.2627. Bibcode:2013ApJ...768...24O. doi:10.1088/0004-637X/768/1/24. Retrieved 12 March 2013.
  15. ↑ Alien planet’s atmosphere contains water and carbon monoxide
  16. ↑ Giant Alien Planet in Supersized Solar System May Solve Mystery

External links

Media related to HR 8799 c at Wikimedia Commons

Coordinates: 23h 07m 28.7150s, +21° 08′ 03.302″

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