From Wikipedia, the free encyclopedia
3 Vulpeculae

A light curve for V377 Vulpeculae, plotted from TESS data [1]
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Vulpecula
Right ascension 19h 22m 50.8856s [2]
Declination +26° 15′ 44.667″ [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: 0.922(124)  mas/ yr [2]
Dec.: −10.270(163)  mas/ yr [2]
Parallax (π)8.9071 ± 0.1685  mas [2]
Distance366 ± 7  ly
(112 ± 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
Mass4.16 [5]  M
Luminosity286+64
−52
[7]  L
Surface gravity (log g)4.30 [5]  cgs
Temperature14,343 [5]  K
Rotational velocity (v sin i)15.5 [8] km/s
B
Mass0.6 - 1.1 [5]  M
Age25 [5]  Myr
Other designations
3 Vul, V377 Vulpeculae, BD+25°3811, GC 26748, HD 182255, HIP 95260, HR 7358, SAO 87136 [9]
Database references
SIMBAD data

3 Vulpeculae (abbreviated 3 Vul) is a binary star system in the northern constellation of Vulpecula, [9] located around 366  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. 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.[ 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

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ a b c d e 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.
  3. ^ 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.
  4. ^ 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.
  5. ^ a b c d e f g h i j k l 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.
  6. ^ 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.
  7. ^ 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.
  8. ^ 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.
  9. ^ a b "3 Vul". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-03-13.
  10. ^ Kaler, Jim. "3 Vul". Retrieved 2016-08-09.
  11. ^ 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.
From Wikipedia, the free encyclopedia
3 Vulpeculae

A light curve for V377 Vulpeculae, plotted from TESS data [1]
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Vulpecula
Right ascension 19h 22m 50.8856s [2]
Declination +26° 15′ 44.667″ [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: 0.922(124)  mas/ yr [2]
Dec.: −10.270(163)  mas/ yr [2]
Parallax (π)8.9071 ± 0.1685  mas [2]
Distance366 ± 7  ly
(112 ± 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
Mass4.16 [5]  M
Luminosity286+64
−52
[7]  L
Surface gravity (log g)4.30 [5]  cgs
Temperature14,343 [5]  K
Rotational velocity (v sin i)15.5 [8] km/s
B
Mass0.6 - 1.1 [5]  M
Age25 [5]  Myr
Other designations
3 Vul, V377 Vulpeculae, BD+25°3811, GC 26748, HD 182255, HIP 95260, HR 7358, SAO 87136 [9]
Database references
SIMBAD data

3 Vulpeculae (abbreviated 3 Vul) is a binary star system in the northern constellation of Vulpecula, [9] located around 366  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. 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.[ 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

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ a b c d e 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.
  3. ^ 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.
  4. ^ 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.
  5. ^ a b c d e f g h i j k l 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.
  6. ^ 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.
  7. ^ 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.
  8. ^ 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.
  9. ^ a b "3 Vul". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-03-13.
  10. ^ Kaler, Jim. "3 Vul". Retrieved 2016-08-09.
  11. ^ 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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