Гипс 412
| Данные наблюдения Epoch J2000 Equinox J2000 | |
|---|---|
| Созвездие | Большая Медведица |
| 412 а | |
| Правильное восхождение | 11 час 05 м 22.3101 с [ 1 ] |
| Склонение | +43° 31′ 51.0404″ [ 1 ] |
| Apparent magnitude (V) | 8.68 [ 2 ] |
| Глиз 412 б | |
| Правильное восхождение | 11 час 05 м 30.8856 с [ 3 ] |
| Склонение | +43° 31′ 17.8843″ [ 3 ] |
| Apparent magnitude (V) | 14.45 [ 4 ] |
| Характеристики | |
| Спектральный тип | M1.0V [ 2 ] /M6.0V [ 4 ] |
| U -B Цветовой индекс | +1.16/— [ 5 ] |
| B - V Индекс цвета | +1.54 [ 5 ] /2.08 [ 6 ] |
| Астрометрия | |
| Gliese 412 A | |
| Radial velocity (Rv) | +64.9 ± 0.9[7] km/s |
| Proper motion (μ) | RA: −4410.43±0.78[8] mas/yr Dec.: 942.93±0.70[8] mas/yr |
| Parallax (π) | 203.8876 ± 0.0332 mas[9] |
| Distance | 15.997 ± 0.003 ly (4.9047 ± 0.0008 pc) |
| Absolute magnitude (MV) | 10.34[10] |
| Gliese 412 B | |
| Proper motion (μ) | RA: −4339.891±0.167 mas/yr Dec.: 960.780±0.162 mas/yr |
| Parallax (π) | 203.8323 ± 0.0500 mas[11] |
| Distance | 16.001 ± 0.004 ly (4.906 ± 0.001 pc) |
| Absolute magnitude (MV) | 16.05[10] |
| Details | |
| GJ 412 A | |
| Mass | 0.48[10] M☉ |
| Radius | 0.398±0.009[12] R☉ |
| Surface gravity (log g) | 4.90[13] cgs |
| Temperature | 3,687[13]/ K |
| Metallicity [Fe/H] | -0.43[13] dex |
| Rotational velocity (v sin i) | <3[14] km/s |
| Age | 3[15] Gyr |
| GJ 412 B | |
| Mass | 0.10[10] M☉ |
| Radius | 0.13[15] R☉ |
| Temperature | 2,700[6] K |
| Metallicity [Fe/H] | −0.32[15] dex |
| Rotational velocity (v sin i) | 7.7±1.7[14] km/s |
| Other designations | |
| Database references | |
| SIMBAD | The system |
| A | |
| B | |
  Gliese 412 Location of Gliese 412 in the constellation Ursa Major | |
Gliese 412 - это пара звезд , которые имеют общее правильное движение через пространство и, как полагают, образуют бинарную звездную систему. Пара имеет угловое разделение 31,4 ″ под углом положения 126,1 °. [ 17 ] Они расположены в 15,8 световых года, отдаленные от солнца в созвездий Ursa Major . Оба компонента являются относительно тусклыми красными карликовыми звездами.
Два звездных компонента этой системы имеют прогнозируемое разделение около 152 ат и ось орбитального полузащитника 190 ат. [ 18 ] Первичный имеет около 48% солнечной массы , в то время как вторичная составляет всего 10%. [ 10 ] Первичный имеет прогнозируемую скорость вращения на экваторе менее 3 км/с; Вторичная скорость вращения составляет 7,7 ± 1,7 км/с. [ 14 ]
The primary star was monitored for radial velocity (RV) variations caused by a Jupiter-mass companion in a short-period orbit. It displayed no significant excess of RV variation that could be attributed to a planet.[19] A search of the system using near-infrared speckle interferometry also failed to detect a companion orbiting at distances of 1–10 AU.[20] Nor has a brown dwarf been detected orbiting within this system.[21]
The space velocity components of this system are U = 141, V = –7 and W = 7. They are members of the halo population of the Milky Way galaxy.[14]
X-ray source
[edit]The secondary is a flare star that is referred to as WX Ursae Majoris. It is characterized as a UV Ceti-type variable star that displays infrequent increases in luminosity. This star was observed to flare as early as 1939 by the Dutch astronomer Adriaan van Maanen.[22]
Component B (WX Ursae Majoris) has been identified as an X-ray source, while no significant X-ray emission was detected from component A.[23] This system had not been studied in X-rays prior to ROSAT.[23] The Gaia DR2 release gives a parallax of 204.059 ±0.169 mas for B, indicating a distance of around 16 light-years.[3]
References
[edit]- ^ Jump up to: a b 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.
- ^ Jump up to: a b c d "BD+44 2051". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-13.
- ^ Jump up to: a b c 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.
- ^ Jump up to: a b c "BD+44 2051B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-13.
- ^ Jump up to: a b Nicolet, B. (1978). "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System". Observatory. Bibcode:1978ppch.book.....N.
- ^ Jump up to: a b Casagrande, Luca; et al. (September 2008). "M dwarfs: effective temperatures, radii and metallicities". Monthly Notices of the Royal Astronomical Society. 389 (2): 585–607. arXiv:0806.2471. Bibcode:2008MNRAS.389..585C. doi:10.1111/j.1365-2966.2008.13573.x. S2CID 14353142.
- ^ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. University of Toronto: International Astronomical Union. Bibcode:1967IAUS...30...57E.
- ^ Jump up to: a b van Leeuwen, F. (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
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ Jump up to: a b c d e "The 100 nearest star systems". Research Consortium On Nearby Stars. 2009-09-14. Archived from the original on 2007-11-12. Retrieved 2009-09-14.
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ Schweitzer, Andreas; Passegger, V. M.; Cifuentes, C.; Bejar, V. J. S.; Cortes-Contreras, M.; Caballero, J. A.; del Burgo, C.; Czesla, S.; Kuerster, M.; Montes, D.; Osorio, M. R. Zapatero; Ribas, I.; Reiners, A.; Quirrenbach, A.; Amado, P. J. (May 2019). "The CARMENES search for exoplanets around M dwarfs: Different roads to radii and masses of the target stars". Astronomy & Astrophysics. 625: A68. arXiv:1904.03231. doi:10.1051/0004-6361/201834965. ISSN 0004-6361.
- ^ Jump up to: a b c Soubiran, C.; Bienaymé, O.; Mishenina, T. V.; Kovtyukh, V. V. (March 2008). "Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants". Astronomy and Astrophysics. 480 (1): 91–101. arXiv:0712.1370. Bibcode:2008A&A...480...91S. doi:10.1051/0004-6361:20078788. S2CID 16602121.
- ^ Jump up to: a b c d Delfosse, Xavier; Forveille, Thierry; Perrier, Christian; Mayor, Michel (March 1998). "Rotation and chromospheric activity in field M dwarfs". Astronomy and Astrophysics. 331: 581–595. Bibcode:1998A&A...331..581D.
- ^ Jump up to: a b c Mann, Andrew W.; et al. (May 2015), "How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius", The Astrophysical Journal, 804 (1): 38, arXiv:1501.01635, Bibcode:2015ApJ...804...64M, doi:10.1088/0004-637X/804/1/64, S2CID 19269312, 64.
- ^ "** VBS 18". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-05-05.
- ^ Gould, Andrew; Chanamé, Julio (February 2004). "New Hipparcos-based Parallaxes for 424 Faint Stars". The Astrophysical Journal Supplement Series. 150 (2): 455–464. arXiv:astro-ph/0309001. Bibcode:2004ApJS..150..455G. doi:10.1086/381147. S2CID 8494577.
- ^ Reid, I. Neill; Gizis, John E. (June 1997). "Low-Mass Binaries and the Stellar Luminosity Function". Astronomical Journal. 113: 2246–2269. Bibcode:1997AJ....113.2246R. doi:10.1086/118436.
- ^ Endl, Michael; et al. (September 2006). "Exploring the Frequency of Close-in Jovian Planets around M Dwarfs". The Astrophysical Journal. 649 (1): 436–443. arXiv:astro-ph/0606121. Bibcode:2006ApJ...649..436E. doi:10.1086/506465. S2CID 14461746.
- ^ Leinert, C.; et al. (September 1997). "A search for companions to nearby southern M dwarfs with near-infrared speckle interferometry". Astronomy and Astrophysics. 325: 159–166. Bibcode:1997A&A...325..159L.
- ^ Oppenheimer, B. R.; et al. (April 2001). "A Coronagraphic Survey for Companions of Stars within 8 Parsecs". The Astronomical Journal. 121 (4): 2189–2211. arXiv:astro-ph/0101320. Bibcode:2001AJ....121.2189O. doi:10.1086/319941. S2CID 119092593.
- ^ Джой, Альфред Х. (июнь 1967 г.). «Звездные вспышки». Астрономическое общество тихоокеанских листовок . 10 (456): 41–48. Bibcode : 1967aspl ... 10 ... 41J .
- ^ Jump up to: а беременный Schmitt JHMM; Флеминг Та; Giampapa MS (сентябрь 1995 г.). «Рентгеновский вид звезд с низкой массой в солнечном районе» . Астрофия. Дж . 450 (9): 392–400. Bibcode : 1995Apj ... 450..392S . doi : 10.1086/176149 .
