HD 142415: Difference between revisions
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| volume=426 | issue=1 | pages=484–495 | date=October 2012 |
| volume=426 | issue=1 | pages=484–495 | date=October 2012 |
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| doi=10.1111/j.1365-2966.2012.21730.x | arxiv=1207.4610 |
| doi=10.1111/j.1365-2966.2012.21730.x | doi-access=free | arxiv=1207.4610 |
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| bibcode=2012MNRAS.426..484D | s2cid=118378819 }}</ref> |
| bibcode=2012MNRAS.426..484D | s2cid=118378819 }}</ref> |
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Latest revision as of 02:27, 23 August 2024
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Norma |
| Right ascension | 15h 57m 40.79190s[1] |
| Declination | −60° 12′ 00.9228″[1] |
| Apparent magnitude (V) | 7.33[2] |
| Characteristics | |
| Spectral type | G1V[3] |
| B−V color index | 0.621±0.002[2] |
| Astrometry | |
| Radial velocity (Rv) | −11.60±0.72[2] km/s |
| Proper motion (μ) | RA: −112.801±0.050[1] mas/yr Dec.: −101.835±0.051[1] mas/yr |
| Parallax (π) | 28.1149 ± 0.0328 mas[1] |
| Distance | 116.0 ± 0.1 ly (35.57 ± 0.04 pc) |
| Absolute magnitude (MV) | 4.66[2] |
| Details[4] | |
| Mass | 1.10±0.01 M☉ |
| Radius | 1.04±0.01 R☉ |
| Luminosity | 1.16±0.02 L☉ |
| Surface gravity (log g) | 4.52±0.05[5] cgs |
| Temperature | 5,869±12 K |
| Metallicity [Fe/H] | 0.17±0.02[5] dex |
| Rotation | 9.6 d[6] |
| Rotational velocity (v sin i) | 4.2±0.1[3] km/s |
| Age | 1.6±0.6 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 142415 is a single[6] star in the southern constellation of Norma, positioned next to the southern constellation border with Triangulum Australe and less than a degree to the west of NGC 6025. With an apparent visual magnitude of 7.33,[2] it is too faint to be visible to the naked eye. The distance to this star is 116 light years from the Sun based on parallax, but it is drifting closer with a radial velocity of −12 km/s.[2] It is a candidate member of the NGC 1901 open cluster of stars.[8]
This is an ordinary G-type main-sequence star with a stellar classification of G1V.[3] It has been identified as a solar twin by Datson et al. (2012), which means its physical properties are very similar to the Sun.[9] It has 10% more mass than the Sun but only a 3% larger radius. The star is estimated to be 1.6[4] billion years old and is spinning with a projected rotational velocity of 4.2 km/s.[3] It is radiating 1.16 times the luminosity of the Sun from its photosphere at an effective temperature of 5,869 K.[4]
The star is currently known to have one planet, designated HD 142415 b. This was detected via the radial velocity method and announced in 2004. The orbital period is just over a year, which made a determination of the orbital eccentricity more difficult due to undersampling over part of the orbit, in combination with jitter. The authors chose to pin the eccentricity value to 0.5, although solutions in the range 0.2–0.8 would be equally plausible.[6]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >1.62 MJ | 1.05 | 386.3 ± 1.6 | 0.5(fixed) | — | — |
See also
[edit]References
[edit]- ^ 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.
- ^ a b c d e f Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
- ^ a b c d Torres, G. R.; Quast, G. R.; da Silva, L.; de La Reza, R.; Melo, C. H. F.; Sterzik, M. (December 2006). "Search for associations containing young stars (SACY). I. Sample and searching method". Astronomy and Astrophysics. 460 (3): 695–708. arXiv:astro-ph/0609258. Bibcode:2006A&A...460..695T. doi:10.1051/0004-6361:20065602. S2CID 16080025.
- ^ a b c Bonfanti, A.; et al. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics. 585: A5, 14 pp. arXiv:1511.01744. Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297. S2CID 53971692.
- ^ a b Sousa, S. G.; et al. (November 2018). "SWEET-Cat updated. New homogenous spectroscopic parameters". Astronomy & Astrophysics. 620: 13. arXiv:1810.08108. Bibcode:2018A&A...620A..58S. doi:10.1051/0004-6361/201833350. S2CID 119374557. A58.
- ^ a b c d Mayor, M.; et al. (2004). "The CORALIE survey for southern extra-solar planets XII. Orbital solutions for 16 extra-solar planets discovered with CORALIE". Astronomy and Astrophysics. 415 (1): 391–402. arXiv:astro-ph/0310316. Bibcode:2004A&A...415..391M. doi:10.1051/0004-6361:20034250. S2CID 5233877.
- ^ "HD 142415". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-23.
- ^ Murgas, F.; et al. (April 2013), "Stellar activity as a tracer of moving groups", Astronomy and Astrophysics, 552: A27, arXiv:1302.6935, Bibcode:2013A&A...552A..27M, doi:10.1051/0004-6361/201219483, S2CID 7621053
- ^ Datson, Juliet; et al. (October 2012). "New solar twins and the metallicity and temperature scales of the Geneva-Copenhagen Survey". Monthly Notices of the Royal Astronomical Society. 426 (1): 484–495. arXiv:1207.4610. Bibcode:2012MNRAS.426..484D. doi:10.1111/j.1365-2966.2012.21730.x. S2CID 118378819.
