3 Vulpeculae

From Wikipedia, the free encyclopedia
3 Vulpeculae
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Vulpecula
Right ascension 19h 22m 50.88540s[1]
Declination +26° 15′ 44.6676″[1]
Apparent magnitude (V) 5.18[2]
Characteristics
Spectral type B6 III[3]
B−V color index −0.119±0.001[2]
Variable type SPB[4][5]
Astrometry
Radial velocity (Rv)−14.1±1.1[2] km/s
Proper motion (μ) RA: +1.081[1] mas/yr
Dec.: −10.270[1] mas/yr
Parallax (π)9.0575 ± 0.1967[1] mas
Distance360 ± 8 ly
(110 ± 2 pc)
Absolute magnitude (MV)−0.17[2]
Orbit[4]
Period (P)367.7
Eccentricity (e)0.15
Semi-amplitude (K1)
(primary)		6.8 km/s
Details
A
Mass4.16[4] M☉
Luminosity286+64
−52[6] L☉
Surface gravity (log g)4.30[4] cgs
Temperature14,343[4] K
Rotational velocity (v sin i)15.5[7] km/s
B
Mass0.6 - 1.1[4] M☉
Age25[4] Myr
Other designations
3 Vul, V377 Vulpeculae, BD+25°3811, GC 26748, HD 182255, HIP 95260, HR 7358, SAO 87136[8]
Database references
SIMBADdata

3 Vulpeculae (abbreviated 3 Vul) is a binary star system in the northern constellation of Vulpecula,[8] located around 360 light years away from the Sun.[1] 3 Vulpeculae is its Flamsteed designation. It has been nicknamed "the Observer's Nightmare" (or its Latin free translation, "Spectatori Error Inextricabilis") by some astronomers[9][4] because it is difficult to study as its orbital period is close to a year and it is pulsating with a period close to a day.[4] It is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.18.[2]

The primary member, designated component A, is a most likely a B-type main-sequence star[6] with a stellar classification of B6 III.[3] It has been identified as a slowly pulsating B-type star,[4] and has the variable star designation V377 Vulpeculae. The star has 4.16[4] times the mass of the Sun and is radiating 286[6] times the Sun's luminosity from its photosphere at an effective temperature of 14,343 K.[4] The secondary has an estimated 0.6–1.1 solar masses.[4]

References[]

  1. ^ a b c d e f 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.
  2. ^ 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.
  3. ^ a b Cucchiaro, A.; Macau-Hercot, D.; Jaschek, M.; Jaschek, C. (1977). "Spectral classification from the ultraviolet line features of S2/68 spectra. II - Late B-type stars". Astronomy and Astrophysics Supplement Series. 30: 71. Bibcode:1977A&AS...30...71C.
  4. ^ a b c d e f g h i j k l m Dukes, Robert; Kubinec, William; Kubinec, Angela; Adelman, Saul (2003). "A Photometric and Spectroscopic Study of 3 Vulpeculae: An Observer's Nightmare". The Astronomical Journal. 126 (1): 370. Bibcode:2003AJ....126..370D. doi:10.1086/375463.
  5. ^ Samus, N. N.; et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
  6. ^ a b c Walczak, P.; et al. (December 2012). "Constraints on stellar parameters of the slowly pulsating B star HD 182255 from complex asteroseismology". Astronomische Nachrichten. 333 (10): 1065. arXiv:1212.4643. Bibcode:2012AN....333.1065W. doi:10.1002/asna.201211824. S2CID 116926922.
  7. ^ Zverko, J.; Romanyuk, I.; Iliev, I.; Kudryavtsev, D.; Stateva, I.; Semenko, E. (April 2016). "Stars with discrepant v sin i as derived from the Ca II λ3933 Å and Mg II λ4481 Å lines. V. HD 182255 and HD 214923—SPB stars in binary systems". Astrophysical Bulletin. 71 (2): 199–207. Bibcode:2016AstBu..71..199Z. doi:10.1134/S1990341316020073. S2CID 124871780.
  8. ^ a b "3 Vul". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-03-13.
  9. ^ Kaler, Jim. "3 Vul". Retrieved 2016-08-09.
Retrieved from ""