T Vulpeculae

Last updated
T Vulpeculae
TVulLightCurve.png
A visual band light curve for T Vulpeculae, adapted from Kiss (1998) [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Vulpecula
Right ascension 20h 51m 28.23825s [2]
Declination +28° 15′ 01.8166″ [2]
Apparent magnitude  (V)5.754 [3] (5.41 – 6.09) [4]
Characteristics
Spectral type F5 Ib + A0.8 V [5]
B−V color index +0.616±0.049 [6]
Variable type δ Cep [4]
Astrometry
Radial velocity (Rv)−2.6±0.6 [6] km/s
Proper motion (μ)RA: +3.496 [2] mas/yr
Dec.: −15.087 [2] mas/yr
Parallax (π)1.6738±0.0891  mas [2]
Distance 1,900 ± 100  ly
(600 ± 30  pc)
Absolute magnitude  (MV)−3.19 [5]
Details
T Vul A
Mass 4.9 [5]   M☉
Radius 35.6±4.4 [7]   R☉
Luminosity 1,620 [5]   L☉
Surface gravity (log g)1.75 [8]   cgs
Temperature 6,220 [8]   K
Metallicity [Fe/H]0.01 [9]   dex
Age 120 [9]   Myr
T Vul B
Mass 2.1 [5]   M☉
Other designations
T Vul, AAVSO 2047+27, BD+27° 3890, HD 198726, HIP 102949, HR 7988, SAO 89216 [10]
Database references
SIMBAD data

T Vulpeculae is a possible binary star system in the northern constellation of Vulpecula, near the star Zeta Cygni, close to the pair 31 Vulpeculae and 32 Vulpeculae. [11] It is visible to the naked eye with an apparent visual magnitude that ranges around 5.75. [3] The distance to this system is around 1,900  light years, as determined from its annual parallax shift of 1.67  mas . [2]

A well-studied Classical Cepheid variable and one of the brightest known, [12] the apparent magnitude of T Vulpeculae ranges from 5.41 to 6.09 [4] over a period of 4.435 days. [3] It is a yellow-white hued supergiant of spectral type F5 Ib. [5] The variability of T Vul was discovered in 1885 by Edwin Sawyer. [13] Observations between 1885 and 2003 shows a small but continuous decrease in the period of variability amounting to 0.25 seconds per year. [14]

The companion star was detected in 1992; [12] it is an A-type main-sequence star with a class of A0.8 V and 2.1 times the Sun's mass. [5] Orbital periods of 738 and 1,745 days have been proposed for the pair, although, as of 2015, there remains doubt as to whether this is an actual binary system. [15]

References

  1. ↑ Kiss, Laszlo L. (July 1998). "A photometric and spectroscopic study of the brightest northern Cepheids - I. Observations". Monthly Notices of the Royal Astronomical Society. 297 (3): 825. Bibcode:1998MNRAS.297..825K. doi: 10.1046/j.1365-8711.1998.01559.x .
  2. 1 2 3 4 5 6 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 .
  3. 1 2 3 Evans, Nancy Remage; et al. (July 2015). "Binary Properties from Cepheid Radial Velocities (CRaV)". The Astronomical Journal. 150 (1): 18. arXiv: 1505.05823 . Bibcode:2015AJ....150...13E. doi:10.1088/0004-6256/150/1/13. S2CID   54943097. 13.
  4. 1 2 3 BSJ (4 January 2010). "T Vulpeculae". AAVSO Website. American Association of Variable Star Observers . Retrieved 24 January 2014.
  5. 1 2 3 4 5 6 7 Evans, Nancy Remage; Bond, Howard E.; Schaefer, Gail H.; Mason, Brian D.; et al. (2013). "Binary Cepheids: Separations and Mass Ratios in 5M ⊙ Binaries". Astronomical Journal. 146 (4): 93, 10. arXiv: 1307.7123v1 . Bibcode:2013AJ....146...93E. doi:10.1088/0004-6256/146/4/93. S2CID   34133110.
  6. 1 2 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.
  7. ↑ Gallenne, A.; et al. (May 2012). "Mean angular diameters, distances, and pulsation modes of the classical Cepheids FF Aquilae and T Vulpeculae. CHARA/FLUOR near-infrared interferometric observations". Astronomy & Astrophysics. 541: 5. arXiv: 1203.6682 . Bibcode:2012A&A...541A..87G. doi:10.1051/0004-6361/201219102. S2CID   2424989. A87.
  8. 1 2 Gray, R. O.; et al. (2001). "The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. II. Basic Parameters of Program Stars and the Role of Microturbulence". The Astronomical Journal. 121 (4): 2159. Bibcode:2001AJ....121.2159G. doi: 10.1086/319957 .
  9. 1 2 Marsakov, V. A.; Koval', V. V.; Kovtyukh, V. V.; Mishenina, T. V. (2013). "Properties of the population of classical Cepheids in the Galaxy". Astronomy Letters. 39 (12): 851. Bibcode:2013AstL...39..851M. doi:10.1134/S1063773713120050. S2CID   119788977.
  10. ↑ "HD 198726". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 18 August 2018.
  11. ↑ Moore, Patrick (2000), Exploring the Night Sky with Binoculars, Cambridge University Press, p. 147, ISBN   978-0521793902
  12. 1 2 Evans, Nancy R. (July 1992). "The luminosity of the classical Cepheid T VUL". Astronomical Journal. 104 (1): 216–219. Bibcode:1992AJ....104..216E. doi:10.1086/116232.
  13. ↑ Sawyer, E. F. (1886). "On a new variable star in the Constellation Vulpecula". Astronomische Nachrichten. 113 (16): 265. Bibcode:1886AN....113..265S. doi:10.1002/asna.18861131608.
  14. ↑ Meyer, Ralf (August 2006). "T Vulpeculae: Maximum Times Covering 120 Years Show a Slight, Continuous Period Decrease". Open European Journal on Variable Stars. 46: 1. Bibcode:2006OEJV...46....1M.
  15. ↑ Gallenne, A.; et al. (July 2015). "Robust high-contrast companion detection from interferometric observations. The CANDID algorithm and an application to six binary Cepheids". Astronomy & Astrophysics. 579: 12. arXiv: 1505.02715 . Bibcode:2015A&A...579A..68G. doi: 10.1051/0004-6361/201525917 . A68.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.