V419 Cephei
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cepheus |
| Right ascension | 21h 12m 47.24741s[1] |
| Declination | +60° 05′ 52.8017″[1] |
| Apparent magnitude (V) | +6.62[2] |
| Characteristics | |
| Evolutionary stage | Red supergiant |
| Spectral type | M2 Ib[3] |
| Variable type | Lc[4] |
| Astrometry | |
| Parallax (π) | 0.63 ± 0.29[1] mas |
| Distance | 1,085[5] pc |
| Absolute magnitude (MV) | −5.72[2] |
| Details | |
| Mass | 16.6 ± 2.6[6] M☉ |
| Radius | 590[2] R☉ |
| Luminosity | 58,000[2] L☉ |
| Temperature | 3,700[2] K |
| Age | 10.0[6] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
V419 Cephei (BD + 59 2342 or HIP 104719) is a variable star in the constellation of Cepheus with an average apparent magnitude of 6.62.
Distance
Given its distance, V419 Cephei's Hipparcos-measured parallax of 0.63 ± 0.29 milliarcseconds is not constrained to evaluate its distance. Its most likely distance is 1085 ± 320 parsecs, equal to 3,540 ± 1,035 light years. It is a member of the stellar association Cepheus OB2-A.
Characteristics
V419 Cephei is a red supergiant of spectral type M2I with an effective temperature of 3,700 K. It has a theoretical diameter of 590 times solar. K-band angular diameter measurements equal 5.90 ± 0.70 milliarcseconds,[7] which leads to a figure not much higher, although the uncertainty in its distance must also be taken into account. Its has a radius of 2.7 AU. If placed at the Sun's location, it would engulf the orbits of Mercury, Venus, Earth, Mars, and roughly half of the asteroid belt. Despite its large size, it is far smaller than the two supergiants known in this constellation, Mu Cephei and VV Cephei A.
V419 Cephei has a mass 16.6 solar masses, above the limit beyond which stars end their lives as supernovae. The life of such massive stars is very short. Despite its advanced evolutionary state, V419 Cephei is only ~10 million years old.
Billed as an irregular variable star LC, V419 Cephei's brightness varies by 0.27 magnitude.[4]
Reference
- 1 2 3 van Leeuwen, F. (2007). "Validation of the New Hipparcos Reduction". Astronomy and Astrophysics. 474 (2): 653–64. arXiv:0708.1752
. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. - 1 2 3 4 5 Table 4 in Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Josselin, Eric; Maeder, Andre; Meynet, Georges (August 2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not As Cool As We Thought". The Astrophysical Journal. 628 (2): 973–985. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901.
- ↑ Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
- 1 2 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
- ↑ Famaey, B.; Jorissen, A.; Luri, X.; Mayor, M.; Udry, S.; Dejonghe, H.; Turon, C. (2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters". 405. pp. 165-186.
- 1 2 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410: 190. arXiv:1007.4883. Bibcode:2011MNRAS.410..190T. doi:10.1111/j.1365-2966.2010.17434.x.
- ↑ Richichi, A.; Percheron, I.; Khristoforova, M. (2005). "CHARM2: An updated Catalog of High Angular Resolution Measurements". 431 (4). pp. 773-777.