HD 41004
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Pictor |
Right ascension | 05h 59m 49.65018s[1] |
Declination | −48° 14′ 22.8883″[1] |
Apparent magnitude (V) | 8.65[2] (8.82 + 12.51)[3] |
Characteristics | |
Spectral type | K1V + M2V[4] |
B−V color index | 0.887±0.013[2] |
Astrometry | |
Radial velocity (Rv) | +42.36±0.14[1] km/s |
Proper motion ( | RA: −43.418(115) mas/yr[1] Dec.: +65.333(123) mas/yr[1] |
Parallax ( | 25.6106 ± 0.1043 mas[1] |
Distance | 127.4 ± 0.5 ly (39.0 ± 0.2 pc) |
Absolute magnitude (MV) | 5.60[2] |
Details[5] | |
A | |
Mass | 0.89±0.07 M☉ |
Radius | 1.04+0.02 −0.03[6] R☉ |
Luminosity | 0.629±0.008[6] L☉ |
Surface gravity (log g) | 4.34±0.11 cgs |
Temperature | 5,255±52 K |
Metallicity [Fe/H] | 0.15±0.03 dex |
Rotational velocity (v sin i) | 1.0±1.2[7] km/s |
B | |
Mass | 0.4[8] M☉ |
Other designations | |
Database references | |
SIMBAD | data |
HD 41004 is a visual binary[4] star system in the southern constellation of Pictor. It is too faint to be visible to the naked eye, having a combined apparent visual magnitude of 8.65.[2] The two components have a magnitude difference of 3.7, and share a common proper motion[4] with an angular separation of 0.30″, as of 2018.[3] The distance to this system is approximately 127 light-years based on parallax.[1] It is drifting further away from the Sun with a radial velocity of +42.5 km/s, having come to within 44.5 ly some 831,000 years ago.[2]
The primary, component A, is a K-type main-sequence star with a stellar classification of K1V[4] and a visual magnitude of 8.82.[3] Torres et al. (2006) classed it as a K1IV star,[7] suggesting it is a subgiant star that is evolving off the main sequence. It has 89%[4] of the mass of the Sun and 104%[6] of the Sun's radius. The star is radiating 63%[6] of the Sun's luminosity from its photosphere at an effective temperature of 5,255 K.[4] Its smaller companion, designated component B, is a red dwarf with spectral type M2V[4] and apparent magnitude 12.33. It has a projected separation of 23
Companions
[edit]A planet, HD 41004 Ab, was discovered by Zucker et al. and published in 2004. It has a minimum mass 2.56 times that of Jupiter. It orbits the primary star at a separation of 1.70 astronomical units, taking 2.64 years with a high eccentricity of 0.74.[4]
Companion (in order from star) |
Mass | Semimajor axis ( |
Orbital period (days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | ≥2.54±0.74 MJ | 1.70 | 963±38 | 0.74±0.20 | — | — |
HD 41004 Bb is a brown dwarf that at the time of the discovery was orbiting closer to the secondary star than any known extrasolar planet or brown dwarf (a=0.0177
Companion (in order from star) |
Mass | Semimajor axis ( |
Orbital period (days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | ≥18.37±0.22 MJ | 0.0177 | 1.328300(12) | 0.081±0.012 | — | — |
References
[edit]- ^ a b c d e f 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 c d e 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 Mason, B. D.; et al. (2014). "The Washington Visual Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi:10.1086/323920. Retrieved 2015-07-22.
- ^ a b c d e f g h i j k Zucker, S.; et al. (November 2004). "Multi-order TODCOR: Application to observations taken with the CORALIE echelle spectrograph. II. A planet in the system HD 41004". Astronomy and Astrophysics. 426 (2): 695–698. Bibcode:2004A&A...426..695Z. doi:10.1051/0004-6361:20040384.
- ^ 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 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 Torres, C. A. O.; et al. (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.
- ^ Quarles, Billy; Li, Gongjie; Kostov, Veselin; Haghighipour, Nader (2020), "Orbital Stability of Circumstellar Planets in Binary Systems", The Astronomical Journal, 159 (3): 80, arXiv:1912.11019, Bibcode:2020AJ....159...80Q, doi:10.3847/1538-3881/ab64fa, S2CID 209444271
- ^ "HD 41004". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-13.
- ^ Santos, N. C.; et al. (2002). "The CORALIE survey for southern extra-solar planets. IX. A 1.3-day period brown dwarf disguised as a planet". Astronomy and Astrophysics. 392 (1): 215–229. arXiv:astro-ph/0206213. Bibcode:2002A&A...392..215S. doi:10.1051/0004-6361:20020876. S2CID 14195872.
- ^ Narang, Mayank; Manoj, P.; Ishwara Chandra, C. H.; Lazio, Joseph; Henning, Thomas; Tamura, Motohide; Mathew, Blesson; Ujwal, Nitish; Mandal, Pritha (2021), "In search of radio emission from exoplanets: GMRT observations of the binary system HD 41004", Monthly Notices of the Royal Astronomical Society, 500 (4): 4818–4826, arXiv:2011.06843, doi:10.1093/mnras/staa3565
External links
[edit]- "HD 41004 A". Extrasolar Planets Encyclopaedia. Archived from the original on June 2, 2006. Retrieved 2008-07-21.
- "HD 41004 B". Extrasolar Planets Encyclopaedia. Archived from the original on July 2, 2007. Retrieved 2008-07-21.