HD 38858
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| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Orion |
| Right ascension | 05h 48m 34.93996s[1] |
| Declination | −04° 05′ 40.7153″[1] |
| Apparent magnitude (V) | +5.97[2] |
| Characteristics | |
| Spectral type | G4V[3] |
| U−B color index | +0.10[2] |
| B−V color index | +0.64[2] |
| Astrometry | |
| Radial velocity (Rv) | +31.2[4] km/s |
| Proper motion (μ) | RA: 60.84 ± 0.41[1] mas/yr Dec.: –228.35 ± 0.33[1] mas/yr |
| Parallax (π) | 65.89 ± 0.41[1] mas |
| Distance | 49.5 ± 0.3 ly (15.18 ± 0.09 pc) |
| Details | |
| Mass | 0.886[5] M☉ |
| Radius | 0.9331 ± 0.0162[5] R☉ |
| Luminosity | 0.7943 ± 0.0101[5] L☉ |
| Surface gravity (log g) | 4.36 ± 0.06[3] cgs |
| Temperature | 5,660 ± 20[3] K |
| Metallicity [Fe/H] | –0.27 ± 0.03[3] dex |
| Rotational velocity (v sin i) | 2.61[6] km/s |
| Age | 6.2[7] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| Extrasolar Planets Encyclopaedia | data |
HD 38858 is a G-type star[3] with one planet. It's about twice the mass of Uranus and orbits in the star's habitable zone.[8]
The last observation of this system for a dust disc or comet belt was in 2009 by the Spitzer telescope; a belt was inferred at 102 AU.[7] It has an inclination of 48◦.[9]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 32[11] M⊕ | 1.0376 ± 0.0189 | 407.15 ± 4.2857 | 0.27 ± 0.17 | — | — |
| Disk | 102–102 AU | — | — | |||
References
- ↑ 1.0 1.1 1.2 1.3 1.4 van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. Vizier catalog entry
- ↑ 2.0 2.1 2.2 Johnson, H. L.; Iriarte, B.; Mitchell, R. I.; Wisniewskj, W. Z. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory 4 (99). Bibcode:1966CoLPL...4...99J.
- ↑ 3.0 3.1 3.2 3.3 3.4 J. Maldonado, C. Eiroa, E. Villaver, B. Montesinos and A. Mora (2012). "Metallicity of solar-type stars with debris discs and planets". Astronomy & Astrophysics 541. arXiv:1202.5884. Bibcode:2012A&A...541A..40M. doi:10.1051/0004-6361/201218800.
- ↑ Nordström, B. et al. (May 2004). "The Geneva-Copenhagen survey of the Solar neighbourhood: Ages, metallicities, and kinematic properties of 14,000 F and G dwarfs". Astronomy and Astrophysics 418: 989–1019. arXiv:astro-ph/0405198. Bibcode:2004A&A...418..989N. doi:10.1051/0004-6361:20035959.
- ↑ 5.0 5.1 5.2 Boyajian, Tabetha S. et al. (July 2013), "Stellar Diameters and Temperatures. III. Main-sequence A, F, G, and K Stars: Additional High-precision Measurements and Empirical Relations", The Astrophysical Journal 771 (1): 40, arXiv:1306.2974, Bibcode:2013ApJ...771...40B, doi:10.1088/0004-637X/771/1/40.
- ↑ Martínez-Arnáiz, R. et al. (September 2010). "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter". Astronomy and Astrophysics 520: A79. arXiv:1002.4391. Bibcode:2010A&A...520A..79M. doi:10.1051/0004-6361/200913725.
- ↑ 7.0 7.1 Wyatt, M. C. et al. (2012). "Herschel imaging of 61 Vir: implications for the prevalence of debris in low-mass planetary systems". Monthly Notices of the Royal Astronomical Society. arXiv:1206.2370. Bibcode:2012MNRAS.tmp.3237W. doi:10.1111/j.1365-2966.2012.21298.x. citing Lawler et al. 2009, and recalculating its distance.
- ↑ LTT 2380 -- High proper-motion Star, SIMBAD Astronomical Database, accessed 11 October 2012.
- ↑ Bryden et al., promised in John E. Krist, Karl R. Stapelfeldt, Geoffrey Bryden, Peter Plavchan (2012), "Hubble Space Telescope Observations of the HD 202628 Debris Disk", Astronomical Journal, arXiv:1206.2078, Bibcode:2012AJ....144...45K, doi:10.1088/0004-6256/144/2/45
- ↑ "hd_38858_b".
- ↑ Wyatt; m sin i is 0.0961 ± 0.012 MJ / 30.55 ± 4.11 (which Wyatt knew from most current cited paper Mayor, "HARPS XXXIV", 2011). Wyatt has likely factored in the inclination but did not state this outright in the arXiv version of the paper.
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