V345 Carinae

Last updated
V345 Carinae
V345CarLightCurve.png
A light curve for V345 Carinae, plotted from Hipparcos data [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Carina
Right ascension 09h 05m 38.37267s [2]
Declination −70° 32′ 18.5832″ [2]
Apparent magnitude  (V)+4.66 [3] (4.67 to 4.78) [4]
Characteristics
Spectral type B2(IV)n [5]
B−V color index −0.149±0.011 [3]
Variable type Be [6]
Astrometry
Radial velocity (Rv)+19.0±7.4 [3]  km/s
Proper motion (μ)RA: −3.017 [2]   mas/yr
Dec.: +8.394 [2]   mas/yr
Parallax (π)3.2440 ± 0.2602  mas [2]
Distance 1,010 ± 80  ly
(310 ± 20  pc)
Absolute magnitude  (MV)−2.67 [3]
Details
Mass 9.6±0.3 [7]   M☉
Radius 8.70±0.17 [8]   R☉
Luminosity 2,539.73 [3]   L☉
Surface gravity (log g)3.80±0.04 [8]   cgs
Temperature 19,000±190 [8]   K
Rotational velocity (v sin i)140±3 [8]  km/s
Age 20.4±2.3 [7]   Myr
Other designations
E Car, V345 Car, CPD−70°861, GC  12602, HD  78764, HIP  44626, HR  3642, SAO  256583 [9]
Database references
SIMBAD data

V345 Carinae is a star in the constellation Carina. It has the Bayer designation E Carinae; V345 Carinae is the variable star designation. The star has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around +4.66. [3] Its actual brightness varies from magnitude +4.67 to +4.78 with a period of 137.7 days. [4] Based on parallax measurements, it is located at a distance of approximately 1,010  light years from the Sun. [2] It is drifting further away with a radial velocity of around +19 km/s. [3]

This star has a stellar classification of B2(IV)n, [5] matching a suspected B-type subgiant star. The 'n' notation indicates "nebulous" lines caused by rapid rotation: the star is spinning with a projected rotational velocity of 140 km/s. [8] It is a Be star having a circumstellar disk of hot, decreted gas that is inserting emission lines into the spectrum. [6] The star is 20 [7]  million years old with 9.6 [7] times the mass of the Sun and 8.7 [8] times the Sun's radius. It is radiating 2,540 [3] times the luminosity of the Sun from its photosphere at an effective temperature of 19,000 K. [8]

The star displays a complex luminosity variation with a periods of 1.13028 and 137.7 days. Although thought to be a single star, [10] Carrier et al. (2002) suggested the longer period may be caused by some sort of binary interaction with the circumstellar disk or perhaps a light reflecting effect. However, no companion has been detected via radial velocity variations. This suggests that the companion would need to either have less than 1.7 times the mass of the Sun or it is being viewed from nearly pole-on. [11] The short-term variations may be from non-radial pulsations similar to those of ω CMa. [12]

Related Research Articles

18 Andromedae, abbreviated 18 And, is a single star in the northern constellation of Andromeda. 18 Andromedae is the Flamsteed designation. It is visible to the naked eye with an apparent visual magnitude of 5.350. The annual parallax shift of 7.9 mas can be used to estimate a distance of 413 light years. It is moving further from the Earth with a heliocentric radial velocity of +10 km/s.

5 Cancri is a single star in the zodiac constellation of Cancer, located around 520 light years away from the Sun. It is just visible to the naked eye under good seeing conditions as a dim, blue-white hued star with an apparent visual magnitude of 5.99. This object is moving closer to the Sun with a heliocentric radial velocity of −10 km/s.

<span class="mw-page-title-main">28 Cancri</span> Binary star in the constellation Cancer

28 Cancri is a star system in the zodiac constellation of Cancer. It is a variable star with the designation CX Cancri, and is close to the lower limit of visibility with the naked eye, having a mean apparent visual magnitude of 6.05. The annual parallax shift seen from Earth's orbit is 8.5 mas, which provides a distance estimate of about 384 light years. It is moving away from the Sun with a radial velocity of around +9 km/s.

<span class="mw-page-title-main">V337 Carinae</span> Star in the constellation of Carina

V337 Carinae is a K-type bright giant star in the constellation of Carina. It is an irregular variable and has an apparent visual magnitude which varies between 3.36 and 3.44.

HD 90853 is a single star in the southern constellation Carina. It has the Bayer designation s Carinae, while HD 98053 is the identifier from the Henry Draper catalogue. This is a variable star with an apparent visual magnitude that ranges from 3.36 down to 3.51, and thus is bright enough to be visible to the naked eye. It is located at a distance of approximately 1,340 light-years from the Sun based on parallax, and has an absolute magnitude of −4.44. The star is drifting further away with a radial velocity of +9 km/s.

HD 80230 is a single star in the southern constellation of Carina, near the northern constellation border with Vela. It has the Bayer designation g Carinae, while HD 80230 is the star's identifier in the Henry Draper catalogue. This is a suspected variable star with a brightness that has been measured varying from magnitude 4.31 down to 4.35, both of which is bright enough for the star to be visible to the naked eye. The distance to this object is approximately 490 light years based on parallax, but it is drifting closer to the Sun with a radial velocity of −5 km/s.

HD 91942 is a single variable star in the constellation Carina. It has the Bayer designation r Carinae, while HD 91942 is the identifier from the Henry Draper catalogue. This orange-hued object is visible to the naked eye with an apparent visual magnitude of 4.45. Based on parallax measurements, it is located at a distance of approximately 1,180 light years from the Sun. The star has an absolute magnitude of −3.77, and is drifting further away with a radial velocity of +9.9 km/s.

<span class="mw-page-title-main">V344 Carinae</span> Star in the constellation Carina

V344 Carinae is a single star in the southern constellation of Carina. It has the Bayer designation f Carinae, while V344 Carinae is its variable star designation. This star has a blue-white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around 4.50. Historically, it was mentioned in the Almagest, suggesting that some time around 130 BCE it was brighter than its current magnitude. This object is located at a distance of approximately 610 light-years from the Sun based on parallax. The star is drifting further away with a radial velocity of around +27 km/s.

<span class="mw-page-title-main">V520 Carinae</span> Star in the constellation Carina

V520 Carinae is a single star in the southern constellation of Carina. It has the Bayer designation w Carinae, while V520 Carinae is a variable star designation. The star has an orange hue and is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around +4.58. It is located at a distance of approximately 1,140 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +9 km/s. It is a candidate member of the IC 2391 moving group of co-moving stars.

<span class="mw-page-title-main">HD 92063</span> Star in the constellation Carina

HD 92063 is a single star in the southern constellation of Carina. It has the Bayer designation t1 Carinae, while HD 92063 is the star's identifier from the Henry Draper Catalogue. This is a suspected variable star and is visible to the naked eye with an apparent visual magnitude of 5.08. The star is located at a distance of approximately 246 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −10 km/s. Although it appears at the edge of the Carina Nebula, it is much closer than the nebula. It is also not considered a member of the nearby Alessi 5 open cluster of stars.

HD 102776, also known by its Bayer designation j Centauri, is a suspected astrometric binary star system in the southern constellation of Centaurus. It has a blue-white hue and is faintly visible to the naked eye with a typical apparent visual magnitude of 4.30. The distance to this star is approximately 600 light years based on parallax, and it is drifting further away with a radial velocity of ~29 km/s. It is a member of the Lower Centaurus Crux subgroup of the Sco OB2 association. HD 102776 has a relatively large peculiar velocity of 31.1 km/s and is a candidate runaway star that was ejected from its association, most likely by a supernova explosion.

Lambda Geminorum, Latinized from λ Geminorum, is a candidate multiple star system in the constellation Gemini. It is visible to the naked eye at night with a combined apparent visual magnitude of 3.57. The distance to this system is 101 light years based on parallax, and it is drifting closer with a radial velocity of –7.4 km/s. It is a member of what is suspected to be a trailing tidal tail of the Hyades Stream.

<span class="mw-page-title-main">HD 32188</span> Star in the constellation Auriga

HD 32188 is suspected variable star in the northern constellation of Auriga, and is positioned roughly in between Eta and Zeta Aurigae. It has a white hue and is just barely visible to the naked eye with an apparent visual magnitude that fluctuates around 6.08. The distance to this star is approximately 3,000 light years, based on parallax. It has an absolute magnitude of −2.87.

Iota2 Cygni, Latinized from ι2 Cygni and often simply called ι Cygni, is a single star in the constellation Cygnus. It is visible to the naked eye as a white-hued point of light with an apparent visual magnitude of 3.76. Located around 121.3 light-years distant from the Sun based on parallax, it is drifting closer with a radial velocity of −19.5 km/s and is expected to come to within 92 light-years in around 783,000 years.

<span class="mw-page-title-main">64 Eridani</span> Single, yellow-white hued star in the constellation Eridanus

64 Eridani is a single, yellow-white hued star in the constellation Eridanus having variable star designation S Eridani. It is faintly visible to the naked eye with an apparent visual magnitude of 4.77. The annual parallax shift is measured at 12.01 mas, which equates to a distance of about 272 light years. In addition to its proper motion, it is moving closer to the Sun with a radial velocity of around −9 km/s.

g Herculis Star in the constellation Hercules

g Herculis is a binary star system in the northern constellation of Hercules. It has the Flamsteed designation 30 Herculis, while g Herculis is the Bayer designation. This system is visible to the naked eye as a faint, red-hued point of light. Based upon a measured parallax of 9.2 mas, it is located around 354 light years away from the Sun. The system is moving further from the Earth with a heliocentric radial velocity of 1.5 km/s.

<span class="mw-page-title-main">Nu Pegasi</span> Star in the constellation Pegasus

ν Pegasi, Latinized as Nu Pegasi is a single star in the northern constellation of Pegasus. It is an orange-hued star that is faintly visible to the naked eye with an apparent visual magnitude of 4.84. The star is located approximately 261 light years away based on parallax, but is drifting closer with a radial velocity of −19 km/s.

<span class="mw-page-title-main">V1073 Scorpii</span> Variable star in the constellation Scorpius

V1073 Scorpii is a variable star in the constellation Scorpius. It has a non-Greek Bayer designation of k Scorpii. The star has a blue-white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around +4.87. Parallax measurements yield a distance estimate of approximately 2,920 ly (896 pc) from the Sun, and it is drifting further away with a radial velocity of +7 km/s. It has an absolute magnitude of −6.8

<span class="mw-page-title-main">T Ceti</span> Variable star in the constellation Cetus

T Ceti is a semiregular variable star located in the equatorial constellation of Cetus. It varies between magnitudes 5.0 and 6.9 over 159.3 days. The stellar parallax shift measured by Hipparcos is 3.7 mas, which yields a distance estimate of roughly 900 light years. It is moving further from the Earth with a heliocentric radial velocity of +29 km/s.

<span class="mw-page-title-main">8 Draconis</span> White-hued chemically unusual star in the constellation Draco

8 Draconis, formally named Taiyi, is a single star in the northern circumpolar constellation of Draco. Based upon an annual parallax shift of 34.14 mas as seen from the Earth, the star is located approximately 96 light-years from the Sun. It is moving further away with a heliocentric radial velocity of +9 km/s, having come within 40.6 ly some 2.6 million years ago.

References

  1. ↑ "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
  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 . Gaia DR2 record for this source at VizieR.
  3. 1 2 3 4 5 6 7 8 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.
  4. 1 2 "V345 Carinae", Variable Star Index, retrieved 2020-02-19.
  5. 1 2 Houk, Nancy; Cowley, A. P. (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 1, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H.
  6. 1 2 Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID   125853869.
  7. 1 2 3 4 Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv: 1007.4883 , Bibcode:2011MNRAS.410..190T, doi: 10.1111/j.1365-2966.2010.17434.x , S2CID   118629873.
  8. 1 2 3 4 5 6 7 Arcos, C.; et al. (March 2018), "Stellar parameters and H α line profile variability of Be stars in the BeSOS survey", Monthly Notices of the Royal Astronomical Society, 474 (4): 5287–5299, arXiv: 1711.08675 , Bibcode:2018MNRAS.474.5287A, doi: 10.1093/mnras/stx3075 , S2CID   74872624.
  9. ↑ "E Car". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-02-18.
  10. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv: 0806.2878 , Bibcode:2008MNRAS.389..869E, doi: 10.1111/j.1365-2966.2008.13596.x , S2CID   14878976.
  11. ↑ Carrier, F.; et al. (April 2002), "Search for duplicity in periodic variable Be stars", Astronomy and Astrophysics, 385 (2): 488–502, Bibcode:2002A&A...385..488C, doi: 10.1051/0004-6361:20020174 .
  12. ↑ Rivinius, Th.; et al. (November 2003), "Non-radially pulsating Be stars", Astronomy and Astrophysics, 411 (2): 229–247, Bibcode:2003A&A...411..229R, doi: 10.1051/0004-6361:20031285 .
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.