HD 29587
In this article, we will explore the fascinating world of HD 29587 and everything that this concept encompasses. From its origin to its impact on today's society, through its multiple interpretations and applications in different areas, we will delve into this exciting topic that has captured the attention of so many people around the world. Through detailed analysis and careful research, we will discover the different facets of HD 29587 and how it has evolved over time. It doesn't matter if you are an expert on the subject or are simply curious to learn more about it, this article will offer you a complete and enriching vision about HD 29587. Get ready to immerse yourself in this exciting universe!
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Perseus |
| Right ascension | 04h 41m 36.31645s[1] |
| Declination | +42° 07′ 06.4209″[1] |
| Apparent magnitude (V) | 7.29[2] |
| Characteristics | |
| Spectral type | G2 V[3] |
| B−V color index | 0.633[3] |
| Astrometry | |
| Radial velocity (Rv) | +112.67±0.20[1] km/s |
| Proper motion (μ) | RA: +534.004[1] mas/yr Dec.: −414.768[1] mas/yr |
| Parallax (π) | 36.3130±0.0697 mas[1] |
| Distance | 89.8 ± 0.2 ly (27.54 ± 0.05 pc) |
| Absolute magnitude (MV) | 5.08[3] |
| Orbit[4] | |
| Period (P) | 1,474.9±10.2 d |
| Eccentricity (e) | 0.713±0.006[5] |
| Periastron epoch (T) | JD 2,447,763.5±45.8 |
| Argument of periastron (ω) (secondary) | 80.2±13.3° |
| Semi-amplitude (K1) (primary) | 1.02±0.16 km/s |
| Details[3] | |
| Mass | 1.033±0.010[5] M☉ |
| Luminosity | 0.798+0.040 −0.038 L☉ |
| Surface gravity (log g) | 4.54±0.22 cgs |
| Temperature | 5,709±35 K |
| Metallicity | −0.51±0.05 dex |
| Age | 14.7+3.8 −2.7 Gyr |
| Other designations | |
| BD+41° 931, FK5 4419, HD 29587, HIP 21832, SAO 39690, TYC 2901-00064-1, 2MASS J04413631+4207065[6] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
HD 29587 is a Sun-like[7] star with a candidate brown dwarf companion[8] in the northern constellation of Perseus. It has an apparent visual magnitude of 7.29,[2] which means it is too faint to be viewed with the naked eye. Based upon an annual parallax shift of 36.3 mas,[1] it is located 89.8 light years away. The star is moving away from the Earth with a heliocentric radial velocity of +113 km/s,[1] having come to within 55.8 ly some 148,000 years ago.[2] It is a hyper-velocity halo[7] star moving at a rate of 170 km/s relative to the local standard of rest.[9]
This ancient star has a stellar classification of G2 V,[3] matching a G-type main-sequence star. It has 78% of the mass of the Sun and is radiating 80% of the Sun's luminosity from its photosphere at an effective temperature of 5,709 K.[3]
Planetary system
Formerly an IAU radial velocity standard, this star was found to have a variable radial velocity due to a suspected orbiting companion.[8] The a sin i value for the unseen object is 0.0957 ± 0.0108 AU (14.31 ± 1.62 Gm),[4] where a is the semimajor axis and i is the orbital inclination – providing a lower bound for the semimajor axis. The secondary object most likely has a mass in the range 41.0–97.8 MJ, making it a probable brown dwarf.[10]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥ 55.2±9.2[5] MJ | ≥0.0957±0.0108 | 1,474.9±10.2 | 0.356±0.095 | — | — |
References
- ^ a b c d e f g h 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.
- ^ a b c 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 e f Da Silva, Ronaldo; et al. (2015). "Homogeneous abundance analysis of FGK dwarf, subgiant, and giant stars with and without giant planets". Astronomy & Astrophysics. 580: A24. arXiv:1505.01726. Bibcode:2015A&A...580A..24D. doi:10.1051/0004-6361/201525770. S2CID 119216425.
- ^ a b Halbwachs, J. L.; et al. (March 2000). "Exploring the brown dwarf desert with Hipparcos". Astronomy and Astrophysics. 355: 581–594. Bibcode:2000A&A...355..581H.
- ^ a b c Kiefer, F.; et al. (2019), "Detection and characterisation of 54 massive companions with the SOPHIE spectrograph", Astronomy & Astrophysics, 631: A125, arXiv:1909.00739, doi:10.1051/0004-6361/201935113, S2CID 202538098
- ^ "HD 29587". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-08-02.
- ^ a b Fossati, L.; et al. (2017). "The effect of ISM absorption on stellar activity measurements and its relevance for exoplanet studies". Astronomy & Astrophysics. 601: 17. arXiv:1702.02883. Bibcode:2017A&A...601A.104F. doi:10.1051/0004-6361/201630339. S2CID 17549819. A104.
- ^ a b Mazeh; Latham, David W.; Stefanik, Robert P. (1996). "Spectroscopic Orbits for Three Binaries with Low-Mass Companions and the Distribution of Secondary Masses near the Substellar Limit". Astrophysical Journal. 466: 415–427. Bibcode:1996ApJ...466..415M. CiteSeerX 10.1.1.30.5905. doi:10.1086/177521.
- ^ Hobbs, L. M.; Duncan, Douglas K. (June 15, 1987). "The lithium abundance in halo stars". Astrophysical Journal, Part 1. 317: 796–809. Bibcode:1987ApJ...317..796H. doi:10.1086/165328.
- ^ a b Reffert, S.; Quirrenbach, A. (March 2011). "Mass constraints on substellar companion candidates from the re-reduced Hipparcos intermediate astrometric data: nine confirmed planets and two confirmed brown dwarfs". Astronomy & Astrophysics. 527: 22. arXiv:1101.2227. Bibcode:2011A&A...527A.140R. doi:10.1051/0004-6361/201015861. S2CID 54986291. A140.
