  | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Triangulum |
| Right ascension | 01h 48m 41.56269s[1] |
| Declination | +32° 41′ 24.7521″[1] |
| Apparent magnitude (V) | 5.81[2] |
| Characteristics | |
| Spectral type | F8 V[3] |
| U−B color index | −0.03[2] |
| B−V color index | +0.54[2] |
| Astrometry | |
| Radial velocity (Rv) | −24.4±0.3[4] km/s |
| Proper motion (μ) | RA: −167.798 mas/yr[1] Dec.: +296.869 mas/yr[1] |
| Parallax (π) | 36.0886 ± 0.0529 mas[1] |
| Distance | 90.4 ± 0.1 ly (27.71 ± 0.04 pc) |
| Absolute magnitude (MV) | +3.56[5] |
| Details | |
| Mass | 1.11[6] M☉ |
| Radius | 1.67±0.04[7] R☉ |
| Luminosity | 3.228+0.011 −0.010[1] L☉ |
| Surface gravity (log g) | 4.03±0.03[8] cgs |
| Temperature | 6,060±64[7] K |
| Metallicity [Fe/H] | −0.20[9] dex |
| Rotational velocity (v sin i) | 5±3[10] km/s |
| Age | 6.6±0.5[11] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 11007 (LTT 10624; HR 523) is a probable astrometric binary[13] located in the northern constellation Triangulum. The primary is faintly visible to the naked eye as a whitish-yellow-hued star with an apparent magnitude of 5.81.[2] The system is located relatively close at a distance of 90.4 light-years based on Gaia DR3 parallax measurements[1] and it is drifting closer with a heliocentric radial velocity of −24.4 km/s.[4] At its current distance, HD 11007's brightness is diminished by an interstellar extinction of 0.09 magnitudes[14] and it has an absolute magnitude of +3.56.[5] It is moving relatively fast across the celestial sphere,[15] having a high proper motion of 341 mas/yr.[1]
The primary has a stellar classification of F8 V,[3] indicating that it is an ordinary F-type main-sequence star that is generating energy via hydrogen fusion at its core. However, it is slightly evolved, being 1.62 magnitudes above the zero age main sequence.[16] It has 111% the mass of the Sun[6] and a slightly enlarged radius 1.67 times that of the Sun.[7] It is slightly over luminous for its class, radiating 3.23 times the luminosity of the Sun[1] from its photosphere at an effective temperature of 6,060 K.[7] HD 11007 A is metal deficient with an iron abundance that is 63.1% solar[9] and it spins modestly with a somewhat constrained projected rotational velocity of approximately 5 km/s.[10] The system is estimated to be 6.6 billion years old; it was suspected to be part of the thick disk population[11] but is now considered to be one of the older members of the thin disk population.[17]
References
- ^ a b c d e f g h 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 Imagawa, Fumihiko (February 1967). "Observational Results of Three-color Photometry for F-type Stars (II)". Memoirs of the College of Science, University of Kyoto. Series A. 31 (2): 93–100.
- ^ a b Harlan, E. A. (June 1974). "MK classifications for F-and G-type stars. 3". The Astronomical Journal. 79: 682. Bibcode:1974AJ.....79..682H. doi:10.1086/111597. ISSN 0004-6256.
- ^ a b Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35,495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. eISSN 1562-6873. ISSN 1063-7737. S2CID 119231169.
- ^ a b Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN 1562-6873. ISSN 1063-7737. S2CID 119257644.
- ^ a b Lambert, David L.; Reddy, Bacham E. (2004). "Lithium abundances of the local thin disc stars". Monthly Notices of the Royal Astronomical Society. 349 (2): 757–767. arXiv:astro-ph/0401259. Bibcode:2004MNRAS.349..757L. doi:10.1111/j.1365-2966.2004.07557.x. S2CID 118931004.
- ^ a b c d Masana, E.; Jordi, C.; Ribas, I. (10 April 2006). "Effective temperature scale and bolometric corrections from 2MASS photometry". Astronomy & Astrophysics. 450 (2): 735–746. arXiv:astro-ph/0601049. Bibcode:2006A&A...450..735M. doi:10.1051/0004-6361:20054021. eISSN 1432-0746. ISSN 0004-6361. S2CID 15278668.
- ^ Aguilera-Gómez, Claudia; Ramírez, Iván; Chanamé, Julio (June 2018). "Lithium abundance patterns of late-F stars: an in-depth analysis of the lithium desert". Astronomy & Astrophysics. 614: A55. arXiv:1803.05922. Bibcode:2018A&A...614A..55A. doi:10.1051/0004-6361/201732209. eISSN 1432-0746. ISSN 0004-6361. S2CID 62799777.
- ^ a b Mishenina, T; Pignatari, M; Gorbaneva, T; Travaglio, C; Côté, B; Thielemann, F-K; Soubiran, C (October 21, 2019). "Enrichment of the Galactic disc with neutron-capture elements: Mo and Ru". Monthly Notices of the Royal Astronomical Society. 489 (2): 1697–1708. arXiv:1908.02992. Bibcode:2019MNRAS.489.1697M. doi:10.1093/mnras/stz2202. ISSN 0035-8711. S2CID 199511206.
- ^ a b Balachandran, Suchitra (May 1990). "Lithium depletion and rotation in main-sequence stars". The Astrophysical Journal. 354. American Astronomical Society: 310. Bibcode:1990ApJ...354..310B. doi:10.1086/168691. ISSN 0004-637X. S2CID 120769481.
- ^ a b Liu, Wilson M.; Chaboyer, Brian (December 2000). "The Relative Age of the Thin and Thick Galactic Disks". The Astrophysical Journal. 544 (2): 818–829. arXiv:astro-ph/0007193. Bibcode:2000ApJ...544..818L. doi:10.1086/317231. ISSN 0004-637X. S2CID 14270478.
- ^ "HD 11007". SIMBAD. Centre de données astronomiques de Strasbourg.
- ^ Eggleton, P. P.; Tokovinin, A. A. (11 September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869–879. arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. eISSN 1365-2966. ISSN 0035-8711. S2CID 14878976.
- ^ Gontcharov, George A.; Mosenkov, Aleksandr V. (28 September 2017). "Verifying reddening and extinction for Gaia DR1 TGAS main sequence stars". Monthly Notices of the Royal Astronomical Society. 472 (4): 3805–3820. arXiv:1709.01160. Bibcode:2017MNRAS.472.3805G. doi:10.1093/mnras/stx2219. eISSN 1365-2966. ISSN 0035-8711. S2CID 118879856.
- ^ Ivanov, G. A. (June 2002). "Cross-identifications of stars with high proper motion". Kinematika i Fizika Nebesnykh Tel. 18: 287–288. Bibcode:2002KFNT...18..287I. ISSN 0233-7665.
- ^ Nordström, B.; Mayor, M.; Andersen, J.; Holmberg, J.; Pont, F.; Jørgensen, B. R.; Olsen, E. H.; Udry, S.; Mowlavi, N. (16 April 2004). "The Geneva-Copenhagen survey of the Solar neighbourhood". Astronomy & Astrophysics. 418 (3): 989–1019. arXiv:astro-ph/0405198. Bibcode:2004A&A...418..989N. doi:10.1051/0004-6361:20035959. eISSN 1432-0746. ISSN 0004-6361. S2CID 11027621.
- ^ Mishenina, T. V.; Soubiran, C.; Kovtyukh, V. V.; Korotin, S. A. (May 2004). "On the correlation of elemental abundances with kinematics among galactic disk stars". Astronomy & Astrophysics. 418 (2): 551–562. arXiv:astro-ph/0401234. Bibcode:2004A&A...418..551M. doi:10.1051/0004-6361:20034454. ISSN 0004-6361. S2CID 17514939.
This page was last edited on 1 April 2024, at 04:37