HD 10647

HD 10647 (q1 Eridani) is a 6th-magnitude yellow-white dwarf star, 57 light-years away in the constellation of Eridanus. The star is visible to the unaided eye under very dark skies. It is slightly hotter and more luminous than the Sun, and at 1,750 million years old, it is also younger. An extrasolar planet was discovered orbiting this star in 2003.

This article is about q1 Eridani. For other stars with this Bayer designation, see q Eridani.
HD 10647
A star chart of the Eridanus constellation showing the position of HD 10647 (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Eridanus
Right ascension  01h 42m 29.3149s[1]
Declination –53° 44′ 26.9912″[1]
Apparent magnitude (V) 5.52[2]
Characteristics
Spectral type F9V[3]
B−V color index 0.551[2]
Astrometry
Radial velocity (Rv)12.9 km/s
Proper motion (μ) RA: 165.832±0.099[1] mas/yr
Dec.: −105.515±0.097[1] mas/yr
Parallax (π)57.6556 ± 0.0737[1] mas
Distance56.57 ± 0.07 ly
(17.34 ± 0.02 pc)
Absolute magnitude (MV)4.32
Details
Mass1.11 ± 0.02[3] M☉
Radius1.10 ± 0.02[3] R☉
Luminosity1.41[3] L☉
Temperature6218 ± 20[3] K
Metallicity [Fe/H]0.00 ± 0.01[3] dex
Rotation10 ± 3[3]
Rotational velocity (v sin i)4.9[3] km/s
Age1.4 ± 0.9[3] Gyr
Other designations
q1 Eridani, 5 G. Eridani, GJ 3109, HR 506, HIP 7978, SAO 232501, CPD−54° 365
Database references
SIMBADdata
Extrasolar Planets
Encyclopaedia		data

Planetary system

In 2003, Michel Mayor's team announced the discovery of a new planet, HD 10647 b, in Paris at the XIX IAP Colloquium Extrasolar Planets: Today & Tormorrow* . The Anglo-Australian Planet Search team initially did not detect the planet in 2004,[4] though a solution was made by 2006.[5] The CORALIE data was finally published in 2013.[3]

The IRAS infrared space telescope detected an excess of infrared radiation from the star, indicating a possible circumstellar disk.[6] Using this data and later observations with the Spitzer Space Telescope, Infrared Space Observatory and the Atacama Pathfinder Experiment implies that the disk is located at 25 Astronomical units and has a thin (0.02 AU), ring-like structure, with the sharp cutoff in the disk suggesting a planet.[7] Additionally, a much longer wavelength suggests the existence of a much wider belt of material, analogous to the Kuiper belt. The hierarchy of this system is somewhat reminiscent of that of Epsilon Eridani, without an inner asteroid belt.

The HD 10647 planetary system[3]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b >0.94 ± 0.08 MJ 2.015 ± 0.011 989.2 ± 8.1 0.15 ± 0.08 — —
Dust disk 25 AU — —
Dust disk 270–330 AU — —
gollark: Also, "use the same train direction" as other people would probably make more sense than "use this train direction".
gollark: You can also remove belts without rotating them.
gollark: Oh, also, rule 12: "Do not rotate belts ..."?
gollark: This seems weird and arbitrary.
gollark: So, for some reason, there seem to be rules requiring a LHD trains and no loops.

References
  1. 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. Decin, G.; et al. (November 2003), "Age Dependence of the Vega Phenomenon: Observations", The Astrophysical Journal, 598 (1): 636–644, arXiv:astro-ph/0308294, Bibcode:2003ApJ...598..636D, doi:10.1086/378800
  3. Marmier, M.; et al. (2013). "The CORALIE survey for southern extrasolar planets XVII. New and updated long period and massive planets". Astronomy and Astrophysics. 551. A90. arXiv:1211.6444. Bibcode:2013A&A...551A..90M. doi:10.1051/0004-6361/201219639.
  4. Jones, H. R. A.; et al. (2004). "HD10647 and the Distribution of Exoplanet Properties with Semi-major Axis". Extrasolar Planets: Today and Tomorrow. 321: 298. Bibcode:2004ASPC..321..298J.
  5. Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701.
  6. Stencel and Backman; Backman, Dana E. (1991). "A survey for infrared excesses among high galactic latitude SAO stars". The Astrophysical Journal Supplement Series. 75: 905–924. Bibcode:1991ApJS...75..905S. doi:10.1086/191553.
  7. Liseau; et al. (2008). "q1 Eridani: a solar-type star with a planet and a dust belt". Astronomy and Astrophysics Letters. 480 (3): L47–L50. arXiv:0803.1294. Bibcode:2008A&A...480L..47L. doi:10.1051/0004-6361:20079276.

This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.