 A light curve for V377 Vulpeculae, plotted from TESS data | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Vulpecula |
| Right ascension | 19 22 50.8856 |
| Declination | +26° 15′ 44.667″ |
| Apparent magnitude (V) | 5.18 |
| Characteristics | |
| Spectral type | B6 III |
| B−V color index | −0.119±0.001 |
| Variable type | SPB |
| Astrometry | |
| Radial velocity (Rv) | −14.1±1.1 km/s |
| Proper motion (μ) | RA: 0.922(124) mas/yr Dec.: −10.270(163) mas/yr |
| Parallax (π) | 8.9071 ± 0.1685 mas |
| Distance | 366 ± 7 ly (112 ± 2 pc) |
| Absolute magnitude (MV) | −0.17 |
| Orbit | |
| Period (P) | 367.7 |
| Eccentricity (e) | 0.15 |
| Semi-amplitude (K1) (primary) | 6.8 km/s |
| Details | |
| A | |
| Mass | 4.16 M☉ |
| Luminosity | 286+64 −52 L☉ |
| Surface gravity (log g) | 4.30 cgs |
| Temperature | 14,343 K |
| Rotational velocity (v sin i) | 15.5 km/s |
| B | |
| Mass | 0.6 - 1.1 M☉ |
| Age | 25 Myr |
| Other designations | |
| 3 Vul, V377 Vulpeculae, BD+25°3811, GC 26748, HD 182255, HIP 95260, HR 7358, SAO 87136 | |
| Database references | |
| SIMBAD | data |
3 Vulpeculae (abbreviated 3 Vul) is a binary star system in the northern constellation of Vulpecula, located around 366 light years away from the Sun. 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 Vul has been nicknamed "the Observer's Nightmare" (or its Latin free translation, "Spectatori Error Inextricabilis") by some astronomers 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. 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. Such stars are now collectively known by the term slowly pulsating B-type stars. Its 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.
The primary member, designated component A, is a most likely a B-type main-sequence star with a stellar classification of B6 III. The star has 4.16 times the mass of the Sun and is radiating 286 times the Sun's luminosity from its photosphere at an effective temperature of 14,343 K. The secondary has an estimated 0.6–1.1 solar masses.
References
- "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- 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.
- ^ 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.
- 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.
- ^ "3 Vul". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-03-13.
- Kaler, Jim. "3 Vul". Retrieved 2016-08-09.
- 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. Bibcode:1991PASP..103...49H. doi:10.1086/132794.
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