Astronomy:3 Vulpeculae
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Vulpecula |
| Right ascension | 19h 22m 50.8856s[1] |
| Declination | +26° 15′ 44.667″[1] |
| Apparent magnitude (V) | 5.18[2] |
| Characteristics | |
| Evolutionary stage | main sequence[1] |
| Spectral type | B7V[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: 0.922(124)[1] mas/yr Dec.: −10.270(163)[1] mas/yr |
| Parallax (π) | 8.9071 ± 0.1685[1] mas |
| Distance | 366 ± 7 ly (112 ± 2 pc) |
| Absolute magnitude (MV) | −0.17[2] |
| Orbit[4] | |
| Period (P) | 367.7 days |
| Eccentricity (e) | 0.15 |
| Semi-amplitude (K1) (primary) | 6.8 km/s |
| Details | |
| A | |
| Mass | 4.16[4] M☉ |
| Luminosity | 286+64 −52[6] L☉ |
| Surface gravity (log g) | 4.30[4] cgs |
| Temperature | 14,343[4] K |
| Rotational velocity (v sin i) | 15.5[7] km/s |
| B | |
| Mass | 0.6 - 1.1[4] M☉ |
| Age | 25[4] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
3 Vulpeculae (abbreviated 3 Vul) is a binary star system in the northern constellation of Vulpecula,[8] located around 366 light years away from the Sun.[1] 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.[2]
In 1991 Douglas Hube and Christopher Aikman announced their discovery that 3 Vul's brightness varies.[10] The star has been nicknamed "the Observer's Nightmare" (or its Latin free translation, "Spectatori Error Inextricabilis") by some astronomers[11][4] 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.[4] 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.[10] 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.[12]
The primary member, designated component A, is a most likely a B-type main-sequence star[6] with a stellar classification of B7V.[3] 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
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ 3.0 3.1 Negueruela, I.; Simón-Díaz, S.; De Burgos, A.; Casasbuenas, A.; Beck, P. G. (2024). "The IACOB project: XII. New grid of northern standards for the spectral classification of B-type stars". Astronomy and Astrophysics 690. doi:10.1051/0004-6361/202449298. Bibcode: 2024A&A...690A.176N.
- ↑ 4.00 4.01 4.02 4.03 4.04 4.05 4.06 4.07 4.08 4.09 4.10 4.11 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.
- ↑ 6.0 6.1 6.2 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.
- ↑ 8.0 8.1 "3 Vul". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=3+Vul.
- ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html.
- ↑ 10.0 10.1 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.
- ↑ Kaler, Jim. "3 Vul". http://stars.astro.illinois.edu/sow/3vul.html.
- ↑ Triana, S. A.; Moravveji, E.; Pápics, P. I.; Aerts, C.; Kawaler, S. D.; Christensen-Dalsgaard, J. (September 2015). "The Internal Rotation Profile of the B-type Star KIC 10526294 from Frequency Inversion of its Dipole Gravity Modes". The Astrophysical Journal 810 (1). doi:10.1088/0004-637X/810/1/16. Bibcode: 2015ApJ...810...16T.
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