Astronomy:3 Vulpeculae
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Vulpecula |
| Right ascension | 19h 22m 50.88540s[2] |
| Declination | +26° 15′ 44.6676″[2] |
| Apparent magnitude (V) | 5.18[3] |
| Characteristics | |
| Spectral type | B6 III[4] |
| B−V color index | −0.119±0.001[3] |
| Variable type | SPB[5][6] |
| Astrometry | |
| Radial velocity (Rv) | −14.1±1.1[3] km/s |
| Proper motion (μ) | RA: +1.081[2] mas/yr Dec.: −10.270[2] mas/yr |
| Parallax (π) | 9.0575 ± 0.1967[2] mas |
| Distance | 360 ± 8 ly (110 ± 2 pc) |
| Absolute magnitude (MV) | −0.17[3] |
| Orbit[5] | |
| Period (P) | 367.7 |
| Eccentricity (e) | 0.15 |
| Semi-amplitude (K1) (primary) | 6.8 km/s |
| Details | |
| A | |
| Mass | 4.16[5] M☉ |
| Luminosity | 286+64 −52[7] L☉ |
| Surface gravity (log g) | 4.30[5] cgs |
| Temperature | 14,343[5] K |
| Rotational velocity (v sin i) | 15.5[8] km/s |
| B | |
| Mass | 0.6 - 1.1[5] M☉ |
| Age | 25[5] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
3 Vulpeculae (abbreviated 3 Vul) is a binary star system in the northern constellation of Vulpecula,[9] located around 360 light years away from the Sun.[2] 3 Vulpeculae is its Flamsteed designation. It is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.18.[3]
3 Vul has been nicknamed "the Observer's Nightmare" (or its Latin free translation, "Spectatori Error Inextricabilis") by some astronomers[10][5] because it is difficult to study as its orbital period is close to a year, and additionally it is pulsating with a period close to a day.[5] From a twenty-year spectroscopic study, Hube and Aikman established a 367-day orbital period, and noted the presence of non-radial pulsations in the primary star. From sparse photometry, the authors also established the star's light variability. They suggested that the primary is a member of the 53 Persei class of variable stars.[11] Such stars are now collectively known by the term slowly pulsating B-type stars. It's photometric variation led to a variable star designation, as V377 Vulpeculae, but the non-reproducibility of the light curve made determination of the pulsation period elusive.
Continuous monitoring of the star by the Transiting Exoplanet Survey Satellite has revealed a beat-period phenomenon in the light curve, which causes the luminosity variations to fluctuate in amplitude. The pulsations are non-radial, that is, the star's photosphere varies in shape rather than volume; different parts of the star are expanding and contracting simultaneously. These gravity waves, or g-mode waves, can be indicative of the interior structure of the star.[citation needed]
The primary member, designated component A, is a most likely a B-type main-sequence star[7] with a stellar classification of B6 III.[4] The star has 4.16[5] times the mass of the Sun and is radiating 286[7] times the Sun's luminosity from its photosphere at an effective temperature of 14,343 K.[5] The secondary has an estimated 0.6–1.1 solar masses.[5]
References
- ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 3.4 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ 4.0 4.1 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.
- ↑ 5.00 5.01 5.02 5.03 5.04 5.05 5.06 5.07 5.08 5.09 5.10 5.11 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. doi:10.1086/375463. Bibcode: 2003AJ....126..370D.
- ↑ Samus, N. N. et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1 61 (1): 80–88. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S.
- ↑ 7.0 7.1 7.2 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. doi:10.1002/asna.201211824. Bibcode: 2012AN....333.1065W.
- ↑ 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. doi:10.1134/S1990341316020073. Bibcode: 2016AstBu..71..199Z.
- ↑ 9.0 9.1 "3 Vul". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=3+Vul.
- ↑ Kaler, Jim. "3 Vul". http://stars.astro.illinois.edu/sow/3vul.html.
- ↑ Hube, Douglas P.; Aikman, G. C. L. (1991). "3 Vulpeculae: A non-radial pulsator in a one-year binary system". Publications of the Astronomical Society of the Pacific 103 (659): 49-62. doi:10.1086/132794. Bibcode: 1991PASP..103...49H.
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