HD 10647
Location 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 mas[1]
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☉
Temperature6,218 ± 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

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 1.75 billion years old, it is also younger. An extrasolar planet was discovered orbiting this star in 2003.

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 & Tomorrow* [1]. 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] Out of the 300 nearest Sun-like stars, the disk has the highest fractional luminosity out of all of them.[7] It is unusually bright, but not unusually massive; the lower bound of the mass is 8 times that of the Earth.[7]

The inclination of the disk is relatively high,[8] and the disk is asymmetrical, being more extended in the northeast direction than the southwest.[7] It extends from 34 astronomical units (AU) at the inner edge to 134 AU at the outer edge. The inner edge is sharp, suggesting the existence of a planet that carved out the edge. HD 10647 b, with a semimajor axis of about 2 AU, is too far to be responsible. However, other potential planets may be responsible for this feature.[7]

There is some evidence for an additional, warm asteroid belt-like component further in, at 3 to 10 AU away from the star.[7]

The HD 10647 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b[3] >0.94 ± 0.08 MJ 2.015 ± 0.011 989.2 ± 8.1 0.15 ± 0.08 — —
Dust disk[7] 3–10 AU — —
Dust disk[7] 34–134 AU 76.1 ± 1.0° —

References

  1. ^ a b c d e 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 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, S2CID 16751327
  3. ^ a b c d e f g h i j k 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. S2CID 59467665.
  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. S2CID 119067572.
  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. ^ a b c d e f g Lovell, J. B.; Marino, S.; Wyatt, M. C.; Kennedy, G. M.; MacGregor, M. A.; Stapelfeldt, K.; Dent, B.; Krist, J.; Matrà, L.; Kral, Q.; Panić, O.; Pearce, T. D.; Wilner, D. (2021). "High-resolution ALMA and HST images of q1 Eri: An asymmetric debris disc with an eccentric Jupiter". Monthly Notices of the Royal Astronomical Society. 506 (2): 1978–2001. arXiv:2106.05975. doi:10.1093/mnras/stab1678.
  8. ^ 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. S2CID 7872724.

External links


Constellation of Eridanus
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