HD 43848
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Columba[1] |
| Right ascension | 06h 16m 31.35599s[2] |
| Declination | −40° 31′ 54.8276″[2] |
| Apparent magnitude (V) | 8.65[3] |
| Characteristics | |
| Spectral type | K2 IV[4] |
| Astrometry | |
| Proper motion (μ) | RA: +121.719[2] mas/yr Dec.: +200.617[2] mas/yr |
| Parallax (π) | 26.7558±0.0804 mas[2] |
| Distance | 121.9 ± 0.4 ly (37.4 ± 0.1 pc) |
| Absolute magnitude (MV) | +5.76[1] |
| Details | |
| Mass | 0.98[5] M☉ |
| Radius | 0.87[5] R☉ |
| Luminosity | 0.50[5] L☉ |
| Surface gravity (log g) | 4.55[5] cgs |
| Temperature | 5,140[5] K |
| Metallicity [Fe/H] | +0.31[5] dex |
| Rotational velocity (v sin i) | 2.5[5] km/s |
| Age | 3.7±1.7[3] Gyr |
| Other designations | |
| CD−40°2356, HIP 29804, LTT 2505, NLTT 16340, SAO 217824[6] | |
| Database references | |
| SIMBAD | data |
HD 43848 is a 9th magnitude K-type subgiant star located 122 light-years away in the constellation of Columba. The star is less massive than the Sun.
On October 29, 2008, radial velocity measurements made with the MIKE echelle spectrograph on the 6.5-m Magellan II (Clay) telescope revealed the presence of a companion of at least 25 Jupiter masses orbiting the star.[7] Initially thought to be a brown dwarf, astrometric measurements reveal that the true mass of the object is 120+167
−43 Jupiter masses, implying that it is likely to be a red dwarf star.[8]
See also
References
- ^ a b 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. XHIP record for this object at VizieR.
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b Trevisan, M.; et al. (November 2011), "Analysis of old very metal rich stars in the solar neighbourhood", Astronomy & Astrophysics, 535: A42, arXiv:1109.6304, Bibcode:2011A&A...535A..42T, doi:10.1051/0004-6361/201016056, S2CID 49565866. See table 13.
- ^ Gray, R. O.; et al. (October 2003), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I.", The Astronomical Journal, 126 (4): 2048–2059, arXiv:astro-ph/0308182, Bibcode:2003AJ....126.2048G, doi:10.1086/378365, S2CID 119417105
- ^ a b c d e f g Fuhrmann, Klaus; Chini, Rolf (2021). "On ancient solar-type stars - II". Monthly Notices of the Royal Astronomical Society. 501 (4): 4903. Bibcode:2021MNRAS.501.4903F. doi:10.1093/mnras/staa3942.
- ^ "HD 43848". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2026-01-08.
- ^ Minniti, Dante; et al. (2009), "Low-Mass Companions for Five Solar-Type Stars From the Magellan Planet Search Program", The Astrophysical Journal, 693 (2): 1424–1430, arXiv:0810.5348, Bibcode:2009ApJ...693.1424M, doi:10.1088/0004-637X/693/2/1424, S2CID 119224845
- ^ Sozzetti, A.; Desidera, S. (2010), "Hipparcos preliminary astrometric masses for the two close-in companions to HD 131664 and HD 43848. A brown dwarf and a low-mass star", Astronomy and Astrophysics, 509: A103, arXiv:0909.4454, Bibcode:2010A&A...509A.103S, doi:10.1051/0004-6361/200912717, S2CID 15419641
