30 Vulpeculae

Last updated
30 Vulpeculae
Vulpecula constellation map.svg
Red circle.svg
Location of 30 Vulpeculae (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Vulpecula
Right ascension 20h 44m 52.50423s [1]
Declination 25° 16′ 14.2538″ [1]
Apparent magnitude  (V)4.91 [2]
Characteristics
Spectral type K1 III [3]
U−B color index +1.18 [2]
B−V color index +1.19 [2]
Astrometry
Radial velocity (Rv)+30.00 [4]  km/s
Proper motion (μ)RA: −30.988 [1]   mas/yr
Dec.: −184.648 [1]   mas/yr
Parallax (π)9.3255 ± 0.1537  mas [1]
Distance 350 ± 6  ly
(107 ± 2  pc)
Absolute magnitude  (MV)−0.07 [5]
Orbit [6]
Period (P)2,506±4 d
Eccentricity (e)0.383±0.023
Periastron epoch (T)42511±29  MJD
Argument of periastron (ω)
(secondary)		272±5°
Semi-amplitude (K1)
(primary)		4.69±0.13 km/s
Details
Mass 1.55 [7]   M☉
Radius 21.68+0.47
−0.63 [1]   R☉
Luminosity 173.3±3.3 [1]   L☉
Surface gravity (log g)2.47 [8]   cgs
Temperature 4,498+67
−48 [1]   K
Metallicity [Fe/H]−0.10 [5]   dex
Rotational velocity (v sin i)1.5 [9]  km/s
Age 4.20 [7]   Gyr
Other designations
30 Vul, BD+24°4229, FK5  3657, GC  28920, HD  197752, HIP  102388, HR  7939, SAO  89084 [10]
Database references
SIMBAD data

30 Vulpeculae is a binary star system in the northern constellation of Vulpecula, located mid-way between Epsilon Cygni and a diamond-shaped asterism in Delphinus. It is visible to the naked eye as a faint, orange-hued point of light with an apparent visual magnitude of 4.91. [2] The system is located approximately 350  light years away from the Sun based on parallax, [1] and is drifting further away with a mean radial velocity of +30 km/s. [4] The system has a relatively high proper motion, traversing the celestial sphere at the rate of 0.186  arc seconds per annum. [11]

The variable radial velocity of this system was announced in 1922 by W. W. Campbell. It is a single-lined spectroscopic binary system with an orbital period of 6.86 years and an eccentricity of 0.38. The a sin i value is 149 ± 4  Gm (1.00 ± 0.03  AU ), where a is the semimajor axis and i is the orbital inclination. This provides a lower bound on the true semimajor axis. [6]

The visible component is an aging giant star with a stellar classification of K1 III [3] and an estimated age of 4.20 [7]  billion years old. Having exhausted the supply of hydrogen at its core, the star has expanded to 22 [1] times the Sun's radius. It has 1.55 [7] times the mass of the Sun and is radiating 173 [1] times the Sun's luminosity from its swollen photosphere at an effective temperature of 4,498 K. [1]

Related Research Articles

<span class="mw-page-title-main">Beta Scuti</span> Star in the constellation Scutum

Beta Scuti, Latinized from β Scuti, is a binary star system in the southern constellation Scutum. Based upon an annual parallax shift of 3.56 mas as seen from Earth, it is located approximately 920 light years from the Sun. The primary component has an apparent visual magnitude of +4.22 and is radiating about 1,270 times the luminosity of the Sun from its outer atmosphere at an effective temperature of 4,622 K. This yellow-hued star is a G-type bright giant with a stellar classification of G4 IIa.

<span class="mw-page-title-main">1 Aquarii</span> Binary star in the constellation Aquarius

1 Aquarii is a binary star system in the zodiac constellation of Aquarius, about 257 light years away from the Sun. 1 Aquarii is the Flamsteed designation. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 5.151, located a degree north of the celestial equator. The system is moving closer to the Earth with a heliocentric radial velocity of −41 km/s.

27 Arietis is a binary star system in the northern constellation of Aries. 27 Arietis is the Flamsteed designation. It is a dim, yellow-hued star that is close to the lower limit of what can be viewed with the naked eye, having an apparent visual magnitude is 6.21. The annual parallax shift of 11.64±0.12 mas corresponds to a physical distance of approximately 280 light-years from Earth. It is advancing closer to the Earth with a heliocentric radial velocity of −122.7 km/s, and may come as close as 84 light-years in around 643,000 years.

<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">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">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">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.

HD 3346, also known as V428 Andromedae, is a binary star system in the northern constellation of Andromeda. It is a dim star but visible to the naked eye under suitable viewing conditions, having an apparent visual magnitude of 5.14. The distance to HD 3346 can be determined from its annual parallax shift of 4.72 mas. This yields a range of about 690 light-years. At that distance the brightness of the system is diminished by an extinction of 0.16 magnitude due to interstellar dust. It is moving closer to the Earth with a heliocentric radial velocity of −33 km/s.

6 Persei is a binary star system in the northern constellation of Andromeda. It is faintly visible to the naked eye with an apparent visual magnitude of 5.29. The system is located 182 light years from Earth, as determined from its annual parallax shift of 17.9 mas. It is moving further away with a heliocentric radial velocity of +42 km/s. The system has a relatively high rate of proper motion, traversing the celestial sphere at the rate of 0.386 arcsecond/year.

HD 202951 is a probable binary star system located in the northern constellation of Equuleus. It is near the lower limit of visibility to the naked eye, having an apparent visual magnitude of 5.97. The distance to this system can be estimated from the annual parallax shift of 2.74 mas, yielding a value of roughly 1,190 light years. It is moving closer with a heliocentric radial velocity of −37 km/s.

<span class="mw-page-title-main">Xi Cygni</span> Star in the constellation Cygnus

ξ Cygni is a spectroscopic binary star in the constellation Cygnus. Its apparent magnitude is 3.73 and it is located around 360 parsecs (1,200 ly) away.

26 Vulpeculae is a close binary star system in the northern constellation of Vulpecula, around 644 light years away from the Sun. It is a challenge to view with the naked eye, having an apparent visual magnitude of 6.40. The star is moving closer to the Earth with a heliocentric radial velocity of −63 km/s, and is expected to come within 225 light-years in around 2.6 million years.

HD 175535 is a binary star system in the northern circumpolar constellation of Draco. It has an apparent visual magnitude of 4.92, which is bright enough to be faintly visible to the naked eye. The system is located about 302 light years away, as determined from its annual parallax shift of 10.8 mas. It is moving further from the Earth with a heliocentric radial velocity of +8.5 km/s.

<span class="mw-page-title-main">6 Draconis</span> Binary star system in the constellation Draco

6 Draconis is a single-lined spectroscopic binary star system in the northern constellation of Draco, located about 430 light years away from the Sun. It is visible to the naked eye as an orange-hued star with an apparent visual magnitude of 4.95. The system is moving further from the Earth with a heliocentric radial velocity of 3 km/s.

<span class="mw-page-title-main">1 Geminorum</span> Triple star system in the constellation Gemini

1 Geminorum is a star in the constellation Gemini. Its apparent magnitude is 4.15.

<span class="mw-page-title-main">18 Monocerotis</span> Star in the constellation Monoceros

18 Monocerotis is a binary star system located about half way from Orion's Belt to Procyon, in the equatorial constellation of Monoceros. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.47, and is positioned around 370 light years away from the Sun based on parallax. The system is receding from the Earth with a heliocentric radial velocity of +11 km/s.

<span class="mw-page-title-main">49 Orionis</span> Star in the constellation Orion

49 Orionis is a single star in the equatorial constellation of Orion. It has the Bayer designation d Orionis, while 49 Orionis is the Flamsteed designation. This object is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 4.80. It is located 141 light years away from the Sun based on parallax, but is drifting closer with a radial velocity of −5 km/s.

<span class="mw-page-title-main">56 Pegasi</span> Star in the constellation Pegasus

56 Pegasi is a binary star system in the northern constellation of Pegasus. It is visible to the naked eye with a combined apparent visual magnitude of 4.74. The system is approximately 590 light years away from the Sun based on parallax, but is drifting closer with a radial velocity of −28 km/s. It is listed as a member of the Wolf 630 moving group.

<span class="mw-page-title-main">33 Piscium</span> Star in the constellation Pisces

33 Piscium is a binary star system in the zodiac constellation of Pisces. It is visible to the naked eye with an apparent visual magnitude of 4.61. The distance to this system, as determined from an annual parallax shift of 25.32±0.53 mas, is about 129 light years. It is moving closer to the Sun with a heliocentric radial velocity of −6.6 km/s.

HD 72945 and HD 72946 form a co-moving star system in the northern constellation of Cancer. HD 72945 is a binary star that is dimly visible to the naked eye as a point of light with an apparent visual magnitude of 5.91. At an angular separation of 10.10″ is the fainter companion star HD 72946 at magnitude 7.25. It is being orbited by a brown dwarf. The system as a whole is located at a distance of approximately 84 light years from the Sun based on parallax measurements.

References

  1. 1 2 3 4 5 6 7 8 9 10 11 12 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.
  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 Keenan, P. C.; McNeil, R. C. (1989). "The Perkins catalog of revised MK types for the cooler stars". The Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
  4. 1 2 Famaey, B.; et al. (2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data". Astronomy & Astrophysics. 430: 165–186. arXiv: astro-ph/0409579 . Bibcode:2005A&A...430..165F. doi:10.1051/0004-6361:20041272. S2CID   17804304.
  5. 1 2 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
  6. 1 2 Griffin, R. F. (August 1983). "Spectroscopic binary orbits from photoelectric radial velocities. Paper 51: 30 Vulpeculae". The Observatory. 103: 199–203. Bibcode:1983Obs...103..199G.
  7. 1 2 3 4 Luck, R. Earle (2015). "Abundances in the Local Region. I. G and K Giants". Astronomical Journal. 150 (3). 88. arXiv: 1507.01466 . Bibcode:2015AJ....150...88L. doi:10.1088/0004-6256/150/3/88. S2CID   118505114.
  8. ↑ McWilliam, Andrew (December 1990). "High-resolution spectroscopic survey of 671 GK giants. I - Stellar atmosphere parameters and abundances". Astrophysical Journal Supplement Series. 74: 1075–1128. Bibcode:1990ApJS...74.1075M. doi: 10.1086/191527 .
  9. ↑ De Medeiros, J. R.; et al. (October 2002). "The Rotation of Binary Systems with Evolved Components". The Astrophysical Journal. 578 (2): 943–950. arXiv: astro-ph/0207288 . Bibcode:2002ApJ...578..943D. doi:10.1086/342613. S2CID   16196039.
  10. ↑ "30 Vul". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-06-27.
  11. ↑ Lépine, Sébastien; Shara, Michael M. (March 2005). "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)". The Astronomical Journal. 129 (3): 1483–1522. arXiv: astro-ph/0412070 . Bibcode:2005AJ....129.1483L. doi:10.1086/427854. S2CID   2603568.
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.