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 (μ) | RA: −43.418(115) mas/yr[1] Dec.: 65.333(123) mas/yr[1] |
| Parallax (π) | 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 AU from the primary.[4]
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 (AU) |
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 AU), at only 145 km/s, because of its low-mass parent star, taking 1.3 days. Its orbit is circular despite the gravitational effect of HD 41004 A because of the tidal effect of the nearby star HD 41004 B.[10] A search for cyclotron radiation from the magnetosphere of Bb in 2020 did not find any, indicating the planet is either weakly magnetized, or the emission cone did not point to Earth at the time of observation.[11]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
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.
