1 Vulpeculae

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1 Vulpeculae
Vulpecula constellation map.svg
Red circle.svg
Location of 1 Vulpeculae (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Vulpecula
Right ascension 19h 16m 13.0392s [1]
Declination 21° 23′ 25.544″ [1]
Apparent magnitude  (V)4.77 [2]
Characteristics
Spectral type B4IV [3]
U−B color index -0.54 [2]
B−V color index -0.05 [2]
Astrometry
Radial velocity (Rv)−17.00 [4]  km/s
Proper motion (μ)RA: −0.383±0.141 [1]   mas/yr
Dec.: −5.809±0.152 [1]   mas/yr
Parallax (π)4.2065 ± 0.1557  mas [1]
Distance 780 ± 30  ly
(238 ± 9  pc)
Absolute magnitude  (MV)-2.20 [3]
Details
Mass 6.9 [5]   M☉
Luminosity 919 [3]   L☉
Surface gravity (log g)3.74 [6]   cgs
Temperature 16,787 [6]   K
Metallicity [Fe/H]0.00 [6]   dex
Rotational velocity (v sin i)80 [7]  km/s
Other designations
CCDM  J19162+2123A, BD+21 3713, FK5  3540, GC  26569, GSC 01611-02043, 2MASS J19161302+2123257, HIP  94703, HR  7306, HD  180554, SAO  87010, WDS  J19162+2123A
Database references
SIMBAD data

1 Vulpeculae is a class B4IV [3] (blue subgiant) star in the constellation Vulpecula. Its apparent magnitude is 4.77 [2] and it is approximately 780 light years away based on parallax. [1]

The primary was discovered to be a spectroscopic binary in 1978 with a period around 250 days although the orbital elements are described as marginal. [8] There are also companions B, with magnitude 11.6 and separation 39.1", and C, with magnitude 12.8 and separation 43.6". [9] [10]

Component A is also a suspected variable star, reported to vary from 4.57 to 4.77 in magnitude. [11] It was reported as possibly variable in 1952 during a search for β CMa variables, [12] but has not been seen to vary since. It was listed as one of the least variable stars based on Hipparcos photometry. [13]

On 29 May 1983, 1 Vulpeculae was occulted by the asteroid Pallas. This event was observed at 130 locations in the United States and Mexico and was the best observed of all asteroid occultation events. [14]

Related Research Articles

Rho<sup>1</sup> Sagittarii Star in the constellation Sagittarius

Rho1 Sagittarii, Latinized from ρ1 Sagittarii, is a single, variable star in the southern constellation of Sagittarius. It has a white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around 3.93. The distance to this star is approximately 127 light years based on parallax, and it is drifting further away with a radial velocity of +1.2 km/s. It is positioned near the ecliptic and so it can be occulted by the Moon.

<span class="mw-page-title-main">Rho Serpentis</span> Star in the Serpens constellation

Rho Serpentis, Latinized from ρ Serpentis, is a single star in the Caput section of the equatorial Serpens constellation. It has an orange hue and is faintly visible to the naked eye with an apparent visual magnitude of +4.78. The distance to this star is approximately 375 light years based on parallax, but it is drifting closer to the Sun with a radial velocity of −62 km/s.

Mu<sup>1</sup> Cancri Red giant star in the constellation Cancer

Mu1 Cancri, Latinised from μ1 Cancri, is a variable star in the zodiac constellation of Cancer. The name Mu1 comes from the Bayer naming system: the "1" in the name is because (from Earth) it appears to be close to 10 Cancri, or Mu2 Cancri. It is also known by the variable star designation BL Cancri. The star is dimly visible to the naked eye with an apparent visual magnitude that ranges from 5.87 down to 6.07. Parallax measurements put it about 630 light-years (192 parsecs) from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.28. The position of the star near the ecliptic means it is subject to lunar occultations.

<span class="mw-page-title-main">V533 Carinae</span> Star in the constellation Carina

V533 Carinae is a white A-type supergiant variable star with a mean apparent magnitude of +4.59 in the constellation Carina. It is over 10,000 light years from Earth.

<span class="mw-page-title-main">23 Vulpeculae</span> Star in the constellation Vulpecula

23 Vulpeculae is a triple star system in the northern constellation of Vulpecula. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.52 and it is located approximately 327 light years away from the Sun based on parallax. The system is moving further from the Earth with a heliocentric radial velocity of +1.47 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">29 Vulpeculae</span> Binary star system in the constellation Vulpecula

29 Vulpeculae is a suspected astrometric binary star system in the northern constellation Vulpecula. It is visible to the naked eye as a faint, white-hued point of light with an apparent visual magnitude of 4.82. The system lies approximately 209 light years away from the Sun based on parallax, and is a member of the IC 2391 supercluster. It is moving closer to the Earth with a heliocentric radial velocity of −17 km/s.

<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">V394 Aurigae</span> Star in the constellation Auriga

V394 Aurigae is a semi-regular variable star in the constellation Auriga. Its brightness varies between magnitudes 6.01 and 6.11, so it is faintly visible to the naked eye under ideal observing conditions. Koen and Eyer found that the star's brightness, as seen by Hipparcos, varies with a period of 3.9 days. Located around 730 light-years distant, V394 Aurigae shines with a luminosity approximately 1075 times that of the Sun and has a surface temperature of 3589 K.

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

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<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">28 Monocerotis</span> Star in the constellation Monoceros

28 Monocerotis is a single star in the equatorial constellation of Monoceros. It has an orange-hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.69. The distance to this star is approximately 450 light years based on parallax, and it has an absolute magnitude of −1.00. The star is drifting further away from the Sun with a radial velocity of +26.7 km/s.

<span class="mw-page-title-main">17 Persei</span> Star in the constellation Perseus

17 Persei is a single star in the northern constellation of Perseus, located about 390 light years away from the Sun. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.53. This object is moving further from the Earth at a heliocentric radial velocity of +13 km/s.

Lambda<sup>1</sup> Phoenicis Star in the constellation Phoenix

λ1 Phoenicis, Latinized as Lambda1 Phoenicis, is a double star in the southern constellation of Phoenix. It is visible to the naked eye as a faint, white-hued point of light with a combined apparent visual magnitude of 4.76. The system is located approximately 183 light years away from the Sun based on parallax. It is a member of the Hyades Supercluster.

<span class="mw-page-title-main">QW Puppis</span> F3V star in the constellation Puppis

QW Puppis is a class F3V star in the constellation Puppis. Its apparent magnitude is 4.49 and it is approximately 69.5 light years away based on parallax.

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

1 Puppis is a single star in the southern constellation of Puppis. It lies in the northern part of the constellation at a distance of about 790 ly, east of Aludra in Canis Major and just north of the white supergiant, 3 Puppis. This object is visible to the naked eye as a faint, red-hued star with an apparent visual magnitude of 4.59. It is moving further from the Earth with a heliocentric radial velocity of +32.4 km/s.

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

Y Centauri or Y Cen is a semiregular variable star in the constellation of Centaurus.

<span class="mw-page-title-main">3 Geminorum</span> Star in the constellation Gemini

3 Geminorum is a blue supergiant star in the constellation Gemini. It is a small amplitude pulsating variable and a close double star, with a mean combined apparent visual magnitude of about 5.7.

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

V520 Persei is a blue supergiant member of NGC 869, one of the Perseus Double Cluster open clusters. It is an irregular variable star. At a magnitude of 6.55, V520 Persei is the brightest member in either NGC 869 or NGC 884, although the brighter HD 13994 lies in the foreground along the same line of sight.

References

  1. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 3 4 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  3. 1 2 3 4 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. Vizier catalog entry
  4. ↑ Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Carnegie Institution of Washington. Bibcode:1953GCRV..C......0W. LCCN   54001336.
  5. ↑ Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (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. Vizier catalog entry
  6. 1 2 3 Wu, Yue; Singh, H. P.; Prugniel, P.; Gupta, R.; Koleva, M. (2010). "Coudé-feed stellar spectral library – atmospheric parameters". Astronomy & Astrophysics. 525: A71. arXiv: 1009.1491 . Bibcode:2011A&A...525A..71W. doi:10.1051/0004-6361/201015014. S2CID   53480665.
  7. ↑ Abt, Helmut A.; Levato, Hugo; Grosso, Monica (2002). "Rotational Velocities of B Stars". The Astrophysical Journal. 573 (1): 359–365. Bibcode:2002ApJ...573..359A. doi: 10.1086/340590 .
  8. ↑ Abt, H. A.; Levy, S. G. (1978). "Binaries among B2-B5 IV, V absorption and emission stars". The Astrophysical Journal Supplement Series. 36: 241–258. Bibcode:1978ApJS...36..241A. doi:10.1086/190498.
  9. ↑ Dommanget, J.; Nys, O. (2002). "VizieR Online Data Catalog: CCDM (Catalog of Components of Double & Multiple stars) (Dommanget+ 2002)". VizieR On-line Data Catalog: I/274. Originally Published in: Observations et Travaux 54. 1274. Bibcode:2002yCat.1274....0D. Vizier catalog entry
  10. ↑ Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi: 10.1086/323920 . Vizier catalog entry
  11. ↑ 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.
  12. ↑ Walker, M. F. (1952). "A search for stars of the beta Canis Majoris type". Astronomical Journal. 57: 227. Bibcode:1952AJ.....57..227W. doi:10.1086/106759.
  13. ↑ Adelman, S. J. (2001). "Research Note Hipparcos photometry: The least variable stars". Astronomy and Astrophysics. 367: 297–298. Bibcode:2001A&A...367..297A. doi: 10.1051/0004-6361:20000567 .
  14. ↑ Dunham, D. W.; et al. (1990). "The size and shape of (2) Pallas from the 1983 occultation of 1 Vulpeculae". The Astronomical Journal. 99: 1636–1662. Bibcode:1990AJ.....99.1636D. doi: 10.1086/115446 .
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