HAT-P-17

HAT-P-17
Observation data
Epoch J2000      Equinox J2000
Constellation Cygnus[1]
Right ascension 21h 38m 08.7305s[2]
Declination +30° 29′ 19.453″[2]
Apparent magnitude (V) 10.38[3]
Characteristics
Astrometry
Proper motion (μ) RA: −79.859±0.655[2] mas/yr
Dec.: −127.498±0.773[2] mas/yr
Parallax (π)10.85 ± 0.27[2] mas
Distance301 ± 7 ly
(92 ± 2 pc)
Details
Mass0.857±0.039 M☉
Radius0.837 R☉
Luminosity0.48±0.04 L☉
Surface gravity (log g)4.53±0.02[4] cgs
Temperature5345±70[4] K
Metallicity0.06±0.08[4]
Rotational velocity (v sin i)0.56+0.12
−0.14[5] km/s
Age7.8±3.3 Gyr
Other designations
TYC 2717-417-1, GSC 02717-00417
Database references
SIMBADdata

HAT-P-17 is a K-type main-sequence star about 92 parsecs (300 ly)[2] away. It has a mass of about 0.857 ± 0.039 M☉. It is the host of two planets, HAT-P-17b and HAT-P-17c, both discovered in 2012.[6] A search for a binary companion star using adaptive optics at the MMT Observatory was negative.[7] A candidate companion was detected by a spectroscopic search of high-resolution K band infrared spectra taken at the keck observatory.[8]

Planetary system

In 2012 a multi-planet system consisting of a transiting hot Saturn in an eccentric orbit and a Jupiter like planet in an outer orbit. The transiting planet HAT-P-17b was detected by the HATNet Project using telescopes located in Hawaii, Arizona and at Wise Observatory in Israel. It was confirmed with radial velocity measurements taken at the Keck telescope which also led to the discovery of the second planet on a much wider orbit.[6] In 2013 radial velocity measurements of the Rossiter-McLaughlin effect showed that the sky-projected angle between the stellar spin axis and the orbit of planet b was approximately 19°.[5]

The HAT-P-17 planetary system[6][9]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 0.537±0.017 MJ 0.0882+0.0013
−0.0014		 10.338523+0.000088
−0.000089		 0.3417±0.0036 89.20+0.20
−0.10°		 1.010±0.029 RJ
c > 2.88±0.10 MJ 4.67±0.14 3972+185
−146		 0.295±0.021 — —

References

  1. ↑ Roman, Nancy G. (1987). "Identification of a Constellation From a Position". Publications of the Astronomical Society of the Pacific. 99 (617): 695–699. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Vizier query form
  2. 1 2 3 4 5 6 Brown, A. G. A; et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy and Astrophysics. 595. A2. arXiv:1609.04172. Bibcode:2016A&A...595A...2G. doi:10.1051/0004-6361/201629512. Gaia Data Release 1 catalog entry
  3. ↑ Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H.
  4. 1 2 3 Torres, Guillermo; et al. (2012). "Improved Spectroscopic Parameters for Transiting Planet Hosts". The Astrophysical Journal. 757 (2). 161. arXiv:1208.1268. Bibcode:2012ApJ...757..161T. doi:10.1088/0004-637X/757/2/161.
  5. 1 2 Fulton, Benjamin J.; et al. (2013). "The Stellar Obliquity and the Long-period Planet in the HAT-P-17 Exoplanetary System". The Astrophysical Journal. 772 (2). 80. arXiv:1301.6289. Bibcode:2013ApJ...772...80F. doi:10.1088/0004-637X/772/2/80.
  6. 1 2 3 Howard, A. W.; et al. (2012). "HAT-P-17b,c: A Transiting, Eccentric, Hot Saturn and a Long-period, Cold Jupiter". The Astrophysical Journal. 749 (2). 134. arXiv:1008.3898. Bibcode:2012ApJ...749..134H. doi:10.1088/0004-637X/749/2/134.
  7. ↑ Adams, E. R.; et al. (2013). "Adaptive Optics Images. II. 12 Kepler Objects of Interest and 15 Confirmed Transiting Planets". The Astronomical Journal. 146 (1). 9. arXiv:1305.6548. Bibcode:2013AJ....146....9A. doi:10.1088/0004-6256/146/1/9.
  8. ↑ Piskorz, Danielle; et al. (2015). "Friends of Hot Jupiters. III. An Infrared Spectroscopic Search for Low-mass Stellar Companions". The Astrophysical Journal. 814 (2). 148. arXiv:1510.08062. Bibcode:2015ApJ...814..148P. doi:10.1088/0004-637X/814/2/148.
  9. ↑ Bonomo, A. S.; et al. (2017). "The GAPS Programme with HARPS-N at TNG . XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets". Astronomy and Astrophysics. 602. A107. arXiv:1704.00373. Bibcode:2017A&A...602A.107B. doi:10.1051/0004-6361/201629882.

Coordinates: 21h 38m 09s, +30° 29′ 19″


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