T Vulpeculae

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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, 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]

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<span class="mw-page-title-main">9 Vulpeculae</span> Star in the constellation Vulpecula

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<span class="mw-page-title-main">SV Vulpeculae</span> Star in the constellation Vulpecula

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<span class="mw-page-title-main">BW Vulpeculae</span> Star in the constellation Vulpecula

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<span class="mw-page-title-main">U Vulpeculae</span> Variable star in the constellation Vulpecula

U Vulpeculae is a variable and binary star in the constellation Vulpecula.

<span class="mw-page-title-main">ER Vulpeculae</span> Variable star in the constellation Vulpecula

ER Vulpeculae is a binary star system in the northern constellation of Vulpecula, abbreviated ER Vul. It is a variable star system with a brightness that ranges from an apparent visual magnitude of 7.27 down to 7.49, which is too faint to be visible to the naked eye. This system is located at a distance of 165 light years from the Sun based on parallax measurements. It is drifting closer with a radial velocity of −25 km/s.

<span class="mw-page-title-main">PU Vulpeculae</span> Variable star in the constellation Vulpecula

PU Vulpeculae is a very slowly evolving symbiotic nova in the northern constellation of Vulpecula, abbreviated PU Vul. It is too faint to be visible to the naked eye, reaching a maximum apparent visual magnitude of 8.7 following a minimum of 16.6. The system is located at a distance of approximately 17,000 light years from the Sun based on parallax measurements.

<span class="mw-page-title-main">QQ Vulpeculae</span> Variable star in the constellation Vulpecula

QQ Vulpeculae is a cataclysmic variable binary star system in the northern constellation of Vulpecula, abbreviated QQ Vul. It has a brightness that fluctuates around an apparent visual magnitude of 14.7, which is too faint to be viewed with the naked eye. The distance to this system is approximately 981 light years based on parallax measurements.

<span class="mw-page-title-main">SU Cygni</span> Variable star system in the constellation Cygnus

SU Cygni is a triple star system in the northern constellation of Cygnus, abbreviated SU Cyg. The primary component of the system is a classical Cepheid variable with a period of 3.8455473 days. The changing luminosity of this star causes the system to vary in brightness from a peak apparent visual magnitude of 6.44 down to magnitude 7.22 over the course of its cycle. The distance to this system is approximately 3,200 light years based on parallax measurements. It is a member of the Turner 9 open cluster of stars.

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.
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