HD 1461

HD 1461

HD 1461 is a G0V class star slightly more massive than the Sun (G2V)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cetus[1]
Right ascension 00h 18m 41.8674s[2]
Declination −08° 03′ 10.8058″[2]
Apparent magnitude (V) 6.46[3]
Characteristics
Spectral type G0V
Apparent magnitude (B) 7.14
Apparent magnitude (J) 5.329
Apparent magnitude (H) 5.041
Apparent magnitude (K) 4.897
U−B color index 0.29
B−V color index 0.68
V−R color index 0.35
R−I color index 0.32
Variable type None
Astrometry
Radial velocity (Rv)−10.7 km/s
Proper motion (μ) RA: 417.875±0.098[2] mas/yr
Dec.: −143.768±0.054[2] mas/yr
Parallax (π)42.6090 ± 0.0557[2] mas
Distance76.5 ± 0.1 ly
(23.47 ± 0.03 pc)
Absolute magnitude (MV)4.63 ± 0.03 [4]
Details
Mass1.05 ± 0.02 [5] M☉
Radius1.2441±0.0305[6] R☉
Luminosity1.1893±0.0476[6] L☉
Surface gravity (log g)4.39 cgs
Temperature5386±60[6] K
Metallicity0.18 ± 0.01 [5]
Age2.0 ± 1.1[5] Gyr
Other designations
32 G. Ceti,[7] BD-08°38, GCRV 50265, Gliese 16.1, HIP 1499, HR 72, LTT 149, NLTT 950, PPM 182101, SAO 128690
Database references
SIMBADdata
Exoplanet Archivedata
ARICNSdata
Extrasolar Planets
Encyclopaedia		data

HD 1461 (32 G. Ceti) is a G0V class star slightly more massive than the Sun (G2V), and located about 76.5 light-years (23.5 parsecs ) away in the constellation of Cetus.

Planetary system

On 14 December 2009, scientists announced the discovery at least one planet orbiting around HD 1461.[8][9] The planet, a super-Earth with a 5.8-day orbit was designated HD 1461 b. The data also contained evidence for additional planets with orbital periods of around 400 and 5000 days but the star showed small variations with similar periods, casting doubt on the interpretation of these signals as being caused by orbiting planets.

In September 2011, a paper was published on the arXiv pre-print server giving an orbital solution incorporating data from the HARPS spectrograph. This solution recovered the previously-known planet HD 1461 b, and an additional planet in a 13.5-day orbit.[10] No mention was made of the proposed 400 and 5000-day candidates. As of June 2014, this paper has not yet been published in a refereed scientific journal.

Other than HD 1461 b, the designations for the planets are inconsistent: in the original paper, Rivera et al. designated the 400 and 5000-day candidates as "c" and "d" respectively, whereas the Mayor et al. (2011) pre-print uses the "c" designation for the 13.5-day planet and does not mention the 400-day or 5000-day planets at all.

HD 1461 b has a mass 6.44 times that of the Earth while HD 1461 c has a mass times 5.59 that of the Earth.[11]

The HD 1461 planetary system[11]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥6.44±0.61 M⊕ 0.0634±0.0022 5.77152±0.00045 <0.131 — —
c ≥5.59±0.73 M⊕ 0.1117±0.0039 13.5052±0.0029 <0.228 — —

See also

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 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.
  3. ↑ "HD 1461". SIMBAD Astronomical Database. Retrieved 2009-12-25.
  4. ↑ Holmberg; et al. (2009). "HD 1461". Geneva-Copenhagen Survey of Solar neighbourhood III. Retrieved 2010-12-04.
  5. 1 2 3 M. Tsantaki1; S. G. Sousa1; V. Zh. Adibekyan1; N. C. Santos1; A. Mortier1; G. Israelian (April 2013). "Deriving precise parameters for cool solar-type stars Optimizing the iron line list?" (PDF): 4.
  6. 1 2 3 von Braun, Kaspar; et al. (2014). "Stellar diameters and temperatures - V. 11 newly characterized exoplanet host stars". Monthly Notices of the Royal Astronomical Society. 438 (3): 2413–2425. arXiv:1312.1792. Bibcode:2014MNRAS.438.2413V. doi:10.1093/mnras/stt2360.
  7. ↑ Gould, B. (1879). "32G Ceti". Uranometria Argentina. Retrieved 2012-05-24.
  8. ↑ Rivera, Eugenio J.; et al. (2010). "A Super-Earth Orbiting the Nearby Sun-like Star HD 1461". The Astrophysical Journal. 708 (2): 1492–1499. arXiv:0912.2566. Bibcode:2010ApJ...708.1492R. doi:10.1088/0004-637X/708/2/1492.
  9. ↑ Tim Stephens (2009-12-14). "New planet discoveries suggest low-mass planets are common around nearby stars". UCSC News. UC Santa Cruz. Archived from the original on 2009-12-23. Retrieved 2009-12-14.
  10. ↑ Mayor; et al. (September 2011). "The HARPS search for southern extra-solar planets XXXIV. Occurrence, mass distribution and orbital properties of super-Earths and Neptune-mass planets". arXiv:1109.2497.
  11. 1 2 Díaz, R. F.; et al. (2016). "The HARPS search for southern extra-solar planets. XXXVIII. Bayesian re-analysis of three systems. New super-Earths, unconfirmed signals, and magnetic cycles". Astronomy and Astrophysics. 585. A134. arXiv:1510.06446. Bibcode:2016A&A...585A.134D. doi:10.1051/0004-6361/201526729.

Coordinates: 00h 18m 41.62s, −8° 03′ 9.5″


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