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Variable star in the constellation Vulpecula
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]
References
^ 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 .
^
a
b
c
d
e
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 .
^
a
b 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 .
^
a
b Watson, Christopher (4 January 2010).
"U Vulpeculae" . AAVSO Website .
American Association of Variable Star Observers . Retrieved 2 August 2015 .
^ 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 .
^
a
b 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 .
^
a
b
c 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 .
^
a
b 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 .
^
a
b 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 .
^
"U Vulpeculae" .
SIMBAD .
Centre de données astronomiques de Strasbourg . Retrieved 2 August 2015 .
^ Müller, G.; Kempf, P. (1898).
"Zwei neue Veränderliche von kurzer Periode" (PDF) . Astronomische Nachrichten (in German). 146 (3): 37–42.
Bibcode :
1898AN....146...37M .
doi :
10.1002/asna.18981460303 .
^ 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 .