U Vulpeculae

Last updated
U Vulpeculae
UVulLightCurve.png
A visual band light curve for U Vulpeculae, adapted from Kiss (1998) [1]
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Vulpecula
Right ascension 19h 36m 37.7281s [2]
Declination 20° 19 58.5692 [2]
Apparent magnitude  (V)6.73 - 7.54 [3]
Characteristics
Spectral type F6Iab-G2 [4]
Variable type δ Cep [3]
Astrometry
Proper motion (μ)RA: 0.906±0.050 [2]   mas/yr
Dec.: −0.960±0.062 [2]   mas/yr
Parallax (π)1.0530 ± 0.0390  mas [2]
Distance 3,100 ± 100  ly
(950 ± 40  pc)
Absolute magnitude  (MV)-3.69 [5]
Orbit [6]
Period (P)2,510 days
Eccentricity (e)0.675
Periastron epoch (T)2444800
Argument of periastron (ω)
(secondary)
353°
Semi-amplitude (K1)
(primary)
3.64 km/s
Details
Mass 6.5 [7]   M
Radius 60 [7]   R
Surface gravity (log g)1.75 - 1.85 [8]   cgs
Temperature 5,655 - 5,965 [8]   K
Metallicity [Fe/H]0.09 [9]   dex
Age 82 [9]   Myr
Other designations
BD+20° 4200, HD  185059, HIP  96458, HR  7458, SAO  87447 [10]
Database references
SIMBAD data

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

It is a classical Cepheid variable and its apparent magnitude ranges from 6.73 to 7.54 over a precise cycle of 7.99 days. [4] Its variable nature was discovered in 1898 at Potsdam Observatory by Gustav Müller and Paul Kempf. [11]

In 1991 a study of radial velocities showed that it U Vulpeculae is a spectroscopic binary and a full orbit with a period of 2510 days (6.9 years) was first calculated in 1996. [12] [7] The secondary star is invisible and is only known from its effect on the motion of the primary. [6]

Related Research Articles

<span class="mw-page-title-main">W Sagittarii</span> Star in the constellation Sagittarius

W Sagittarii is a multiple star system star in the constellation Sagittarius, and a Cepheid variable star.

<span class="mw-page-title-main">RT Aurigae</span> Star in the constellation Auriga

RT Aurigae is a yellow supergiant variable star in the constellation Auriga, about 1,500 light years from Earth.

<span class="mw-page-title-main">HD 95109</span> Star in the constellation Carina

HD 95109 is a Classical Cepheid variable, a type of variable star, in the constellation Carina. Its apparent magnitude is 6.86.

<span class="mw-page-title-main">Y Carinae</span> Star in the constellation Carina

Y Carinae is a Classical Cepheid variable, a type of variable star, in the constellation Carina. Its apparent magnitude varies from 7.53 to 8.48.

<span class="mw-page-title-main">V Centauri</span> Variable star in the constellation Centaurus

V Centauri is a Classical Cepheid variable, a type of variable star, in the constellation Centaurus. It is approximately 2,350 light-years away based on parallax.

<span class="mw-page-title-main">31 Vulpeculae</span> Star in the constellation Vulpecula

31 Vulpeculae is a binary star system in the northern constellation of Vulpecula. It is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 4.56. The system is located approximately 228 light years away from the Sun based on parallax, and it is drifting further away with a radial velocity of +2.25 km/s.

<span class="mw-page-title-main">15 Vulpeculae</span> Star in the constellation Vulpecula

15 Vulpeculae is a variable star in the northern constellation of Vulpecula, located approximately 243 light years away based on parallax. It has the variable star designation NT Vulpeculae; 15 Vulpeculae is the Flamsteed designation. It is visible to the naked eye as a faint, white-hued star with a typical apparent visual magnitude of 4.66. This object is moving closer to the Earth with a heliocentric radial velocity of −26 km/s.

<span class="mw-page-title-main">1 Vulpeculae</span> Star in the constellation Vulpecula

1 Vulpeculae is a class B4IV star in the constellation Vulpecula. Its apparent magnitude is 4.77 and it is approximately 780 light years away based on parallax.

<span class="mw-page-title-main">12 Vulpeculae</span> Star in the constellation Vulpecula

12 Vulpeculae is a star in the northern constellation of Vulpecula, located approximately 630 light years away based on parallax. It has the variable star designation V395 Vul; 12 Vulpeculae is the Flamsteed designation. This object is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 4.928. It is moving closer to the Earth with a heliocentric radial velocity of -25 km/s.

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

9 Vulpeculae is a star in the northern constellation of Vulpecula, located about 560 light years away based on parallax. It is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.01. The star is moving further from the Earth with a heliocentric radial velocity of +5 km/s.

<span class="mw-page-title-main">V636 Scorpii</span> Spectroscopic binary star system in the constellation Scorpius

V636 Scorpii is a multiple star system in the constellation Scorpius, 3,000 light years away. The primary is a Classical Cepheid variable and its visual magnitude varies from 6.4 to 6.9.

<span class="mw-page-title-main">U Aquilae</span> Variable binary star system in the constellation Aquila

U Aquilae is a binary star system in the constellation Aquila, Located approximately 614 parsecs (2,000 ly) away from Earth.

<span class="mw-page-title-main">TT Aquilae</span> Star in the constellation Aquila

TT Aquilae is a Classical Cepheid variable star in the constellation Aquila.

<span class="mw-page-title-main">22 Vulpeculae</span> Binary star system in the constellation Vulpecula

22 Vulpeculae is a binary star system in the northern constellation Vulpecula. Based on its parallax, it is located some 1,490 light-years away, and it has an apparent magnitude of about 5.2, making it visible to the naked eye. The system is moving closer to the Earth with a heliocentric radial velocity of −23 km/s.

106 Herculis is a variable star in the northern constellation Hercules. It is visible to the naked eye as a faint, red-hued point of light with a baseline apparent visual magnitude of 4.96. Based on its parallax, it is estimated to lie 383 light-years away from the Sun. The star is moving closer to the Earth with a heliocentric radial velocity of -35 km/s.

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

S Vulpeculae is a variable star located in the constellation Vulpecula. A supergiant star, it is around 382 times the diameter of the Sun.

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

SV Vulpeculae is a classical Cepheid variable star in the constellation Vulpecula. It is a supergiant at a distance of 8,700 light years.

<span class="mw-page-title-main">U Microscopii</span> Star in the constellation Microscopium

U Microscopii is a Mira variable star in the constellation Microscopium. It ranges from magnitude 7 to 14.4 over a period of 334 days. The Astronomical Society of Southern Africa in 2003 reported that observations of U Microscopii were very urgently needed as data on its light curve was incomplete.

<span class="mw-page-title-main">V473 Lyrae</span> Star in the constellation Lyra

V473 Lyrae is a variable star in the constellation Lyra. It is an unusual Classical Cepheid variable with a visual range of 5.99 to 6.35.

<span class="mw-page-title-main">R Puppis</span> Variable star in the constellation Puppis

R Puppis is a variable star in the constellation Puppis. It is a rare yellow hypergiant and a candidate member of the open cluster NGC 2439. It is also an MK spectral standard for the class G2 0-Ia.

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 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 . Gaia DR2 record for this source at VizieR.
  3. 1 2 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
  4. 1 2 Watson, Christopher (4 January 2010). "U Vulpeculae". AAVSO Website. American Association of Variable Star Observers . Retrieved 2 August 2015.
  5. Kovtyukh, V. V.; Chekhonadskikh, F. A.; Luck, R. E.; Soubiran, C.; Yasinskaya, M. P.; Belik, S. I. (2010). "Accurate luminosities for F-G supergiants from FeII/FeI line depth ratios" (PDF). Monthly Notices of the Royal Astronomical Society. 408 (3): 1568. Bibcode:2010MNRAS.408.1568K. doi: 10.1111/j.1365-2966.2010.17217.x .
  6. 1 2 Groenewegen, M. A. T. (2008). "Baade-Wesselink distances and the effect of metallicity in classical cepheids". Astronomy and Astrophysics. 488 (1): 25–35. arXiv: 0807.1269 . Bibcode:2008A&A...488...25G. doi:10.1051/0004-6361:200809859. S2CID   13871801.
  7. 1 2 3 Imbert, M. (1996). "Cepheids and binarity. II. Radial velocities and spectroscopic orbits of four galactic Cepheids: RX Camelopardalis, MW Cygni, Z Lacertae and U Vulpeculae". Astronomy and Astrophysics Supplement (in French). 116: 497–514. Bibcode:1996A&AS..116..497I. doi: 10.1051/aas:1996312 .
  8. 1 2 Andrievsky, S. M.; Lépine, J. R. D.; Korotin, S. A.; Luck, R. E.; Kovtyukh, V. V.; MacIel, W. J. (2013). "Barium abundances in Cepheids". Monthly Notices of the Royal Astronomical Society. 428 (4): 3252. arXiv: 1210.6211 . Bibcode:2013MNRAS.428.3252A. doi: 10.1093/mnras/sts270 .
  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. "U Vulpeculae". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2 August 2015.
  11. Müller, G.; Kempf, P. (1898). "Zwei neue Veränderliche von kurzer Periode". Astronomische Nachrichten (in German). 146 (3): 37–42. Bibcode:1898AN....146...37M. doi:10.1002/asna.18981460303.
  12. Szabados, L. (1991). "Northern Cepheids: Period Update and Duplicity Effects". Communications of the Konkoly Observatory. 11 part 3 (96): 123–244. Bibcode:1991CoKon..96..123S.