PV Cephei

Last updated

PV Cephei
A changing fan.jpg
PV Cep is the bright spot located at the edge of Gyulbudaghian’s Nebula
Credit: ESA/Hubble & NASA. Acknowledgement: Alexey Romashin
Observation data
Epoch J2000        Equinox J2000
Constellation Cepheus [1]
Right ascension 20h 45m 53.943s [2]
Declination +67° 57′ 38.66″ [2]
Apparent magnitude  (V)14.58 - 18.08 [3]
Characteristics
Spectral type A5Ve [4]
Variable type T Tau [5]
Astrometry
Proper motion (μ)RA: 8.228 [6]   mas/yr
Dec.: −1.976 [6]   mas/yr
Parallax (π)2.9100 ± 0.0593  mas [6]
Distance 1,120 ± 20  ly
(344 ± 7  pc)
Details
Mass 2.6 [7]   M☉
Radius 2.9 [7]   R☉
Luminosity 1 [8] - 100 [3]   L☉
Temperature 8,150 [8]   K
Age <1 [3]   Myr
Database references
SIMBAD data

PV Cephei is variable star of Orion type located in the constellation of Cepheus at a distance of over 1600 light-years from Earth. [1]

A red band light curve for PV Cephei, adapted from Lorenzetti et al. (2011) PVCepLightCurve.png
A red band light curve for PV Cephei, adapted from Lorenzetti et al. (2011)

Related Research Articles

<span class="mw-page-title-main">Gamma Cephei</span> Binary star system in the constellation Cephei

Gamma Cephei is a binary star system approximately 45 light-years away in the constellation of Cepheus. The primary is a stellar class K1 orange giant or subgiant star; it has a red dwarf companion. An exoplanet has been confirmed to be orbiting the primary.

<span class="mw-page-title-main">Gliese 105</span> Triple star system in the constellation Cetus

Gliese 105 is a triple star system in the constellation of Cetus. It is located relatively near the Sun at a distance of 23.6 light-years. Despite this, even the brightest component is barely visible with the unaided eye (see Bortle scale). No planets have yet been detected around any of the stars in this system.

<span class="mw-page-title-main">Zeta Cephei</span> Star in the constellation Cepheus

Zeta Cephei is a star in the constellation of Cepheus. Zeta Cephei marks the left shoulder of Cepheus, the King of Joppa (Ethiopia). It is one of the fundamental stars of the MK spectral sequence, defined as type K1.5 Ib.

<span class="mw-page-title-main">V381 Cephei</span> Triple star system in the constellation Cepheus

V381 Cephei is a triple star system in the northern constellation of Cepheus. Its apparent magnitude is slightly variable between 5.5 and 5.7.

<span class="mw-page-title-main">1 Camelopardalis</span> Double star system in the constellation Camelopardalis

1 Camelopardalis is a double star system in the constellation Camelopardalis. Its combined apparent magnitude is 5.56 and it is approximately 800 parsecs (2,600 ly) away.

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

9 Cephei, also known as V337 Cephei, is a variable star in the constellation Cepheus.

<span class="mw-page-title-main">WR 148</span> Binary star in the constellation of Cygnus

WR 148 is a spectroscopic binary in the constellation Cygnus. The primary star is a Wolf–Rayet star and one of the most luminous stars known. The secondary has been suspected of being a stellar-mass black hole but may be a class O main sequence star.

<span class="mw-page-title-main">QZ Puppis</span> Star in the constellation Puppis

QZ Puppis is a class B2.5V star in the constellation Puppis. Its apparent magnitude is 4.5 and it is approximately 650 light years away based on parallax.

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

KQ Puppis is a spectroscopic binary variable star in the constellation Puppis. A red supergiant star and a hot main sequence star orbit each other every 9,742 days. Its apparent magnitude varies between 4.82 and 5.17.

<span class="mw-page-title-main">WR 20a</span> Star in the constellation Carina

WR 20a is an eclipsing binary star belonging to or recently ejected from the young, massive cluster Westerlund 2. It was discovered in 2004 to be one of the most massive binary systems known, for which the masses of the components have been accurately measured.

<span class="mw-page-title-main">EV Carinae</span> Red supergiant star in the constellation Carina

EV Carinae is a red supergiant and pulsating variable star of spectral type M4Ia in the constellation Carina. It is a semiregular variable star with its apparent magnitude varying between 7.4 and 9.0 in the visible band, making it only seen by binoculars or a telescope. Various periods have been identified, but the dominant one is around 347 days. It is an MK spectral standard star for the class M4.5Ia.

<span class="mw-page-title-main">V419 Cephei</span> Star in the constellation Cepheus

V419 Cephei is an irregular variable star in the constellation of Cepheus with an apparent magnitude that varies between 6.54 and 6.89.

<span class="mw-page-title-main">S Cassiopeiae</span> Star in the constellation Cassiopeia

S Cassiopeiae is a Mira variable and S-type star in the constellation Cassiopeia. It is an unusually cool star, rapidly losing mass and surrounded by dense gas and dust producing masers.

<span class="mw-page-title-main">WR 86</span>

WR 86 is a visual binary in the constellation Scorpius consisting of a Wolf-Rayet star and a β Cephei variable. It lies 2° west of NGC 6357 on the edge of the Great Rift in the Milky Way in the tail of the Scorpion.

<span class="mw-page-title-main">II Lupi</span> Star in the constellation Lupus

II Lupi is a Mira variable and carbon star located in the constellation Lupus. It is the brightest carbon star in the Southern Hemisphere at 12 μm.

QV Andromedae is an Alpha2 Canum Venaticorum variable in the constellation Andromeda. Its maximum apparent visual magnitude is 6.6, so it can be seen by the naked eye under very favourable conditions. The brightness varies slightly following a periodic cycle of approximately 5.23 days.

<span class="mw-page-title-main">CC Andromedae</span> Star in the constellation Andromeda

CC Andromedae is a variable star in the constellation Andromeda. It is a pulsating star of the Delta Scuti type, with an apparent visual magnitude that varies between 9.19 and 9.46 with a periodicity of 3 hours.

DH Tauri, also known as DH Tau, is a type M star, located 140 parsecs away. It forms a binary system with DI Tauri 15″ away, and has a substellar companion, either a brown dwarf or massive exoplanet.

SP77 46-44 is a red supergiant star found in the Large Magellanic Cloud in the constellation of Dorado. It is one of the largest stars discovered, with a radius over 1,200 solar radii. If placed in the Solar System, its photosphere would engulf the orbit of Jupiter.

<span class="mw-page-title-main">QY Puppis</span> Red supergiant star in the constellation of Puppis

QY Puppis is a K-type supergiant star in the constellation of Puppis. With a radius of 515 R☉, it is on the smaller end of the largest known stars.

References

  1. 1 2 "A changing fan". ESA/Hubble Picture of the Week. Retrieved 23 April 2013.
  2. 1 2 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  3. 1 2 3 Kun, M.; Szegedi-Elek, E.; Moór, A.; Kóspál, Á.; Ábrahám, P.; Apai, D.; Kiss, Z. T.; Klagyivik, P.; Magakian, T. Yu.; Mező, Gy.; Movsessian, T. A.; Pál, A.; Rácz, M.; Rogers, J. (2011). "Inner disc rearrangement revealed by dramatic brightness variations in the young star PV Cep". Monthly Notices of the Royal Astronomical Society. 413 (4): 2689. arXiv: 1101.2329 . Bibcode:2011MNRAS.413.2689K. doi:10.1111/j.1365-2966.2011.18341.x. S2CID   118623750.
  4. ↑ Watson, C. L. (2006). "The International Variable Star Index (VSX)". The Society for Astronomical Sciences 25th Annual Symposium on Telescope Science. Held May 23–25. 25: 47. Bibcode:2006SASS...25...47W.
  5. ↑ 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. Bibcode:2009yCat....102025S.
  6. 1 2 3 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.
  7. 1 2 Caratti o Garatti, A.; Garcia Lopez, R.; Weigelt, G.; Tambovtseva, L. V.; Grinin, V. P.; Wheelwright, H.; Ilee, J. D. (2013). "LBT/LUCIFER near-infrared spectroscopy of PV Cephei. An outbursting young stellar object with an asymmetric jet". Astronomy and Astrophysics. 554: A66. arXiv: 1304.6267 . Bibcode:2013A&A...554A..66C. doi:10.1051/0004-6361/201321418. S2CID   46977755.
  8. 1 2 Vioque, M.; Oudmaijer, R. D.; Baines, D.; Mendigutía, I.; Pérez-Martínez, R. (2018). "Gaia DR2 study of Herbig Ae/Be stars". Astronomy and Astrophysics. 620: A128. arXiv: 1808.00476 . Bibcode:2018A&A...620A.128V. doi:10.1051/0004-6361/201832870. S2CID   118928804.
  9. ↑ Lorenzetti, D.; Giannini, T.; Larionov, V. M.; Arkharov, A. A.; Antoniucci, S.; Di Paola, A.; Konstantinova, T. S.; Kopatskaya, E. N.; Li Causi, G.; Nisini, B. (May 2011). "Simultaneous monitoring of the photometric and polarimetric activity of the young star PV Cep in the optical/near-infrared bands". The Astrophysical Journal. 732 (2). arXiv: 1103.0183 . doi:10.1088/0004-637X/732/2/69 . Retrieved 6 December 2021.


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.