29 Persei

Last updated
29 Persei
Perseus constellation map.svg
Red circle.svg
Location of 29 Persei (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Perseus
Right ascension 03h 18m 37.74077s [1]
Declination 50° 13 19.8341 [1]
Apparent magnitude  (V)5.16 [2]
Characteristics
Evolutionary stage Main sequence
Spectral type B3V [3]
U−B color index −0.56 [4]
B−V color index −0.06 [4]
Astrometry
Radial velocity (Rv)−1.50 [5]  km/s
Proper motion (μ)RA: +23.574 [1]   mas/yr
Dec.: −24.407 [1]   mas/yr
Parallax (π)5.12 ± 0.29  mas [1]
Distance 640 ± 40  ly
(200 ± 10  pc)
Absolute magnitude  (MV)−1.31 [6]
Details
Mass 6.8 [7]   M
Radius 3.9 [8]   R
Luminosity 960 [6]   L
Surface gravity (log g)4.025±0.113 [9]   cgs
Temperature 16,143 [6]   K
Metallicity [Fe/H]0.00 [10]   dex
Rotational velocity (v sin i)120 [11]  km/s
Other designations
29 Per, BD+49°899, FK5  2188, GC  3934, HD  20365, HIP  15404, HR  987, SAO  23944 [12]
Database references
SIMBAD data
29 Persei is the bright star in the center of this optical light image. 31 Persei is the bright star lower and to the left of 29 Persei. 29 Persei.jpg
29 Persei is the bright star in the center of this optical light image. 31 Persei is the bright star lower and to the left of 29 Persei.

29 Persei is a single [13] star in the northern constellation of Perseus, located approximately 640 light years away from the Sun based on parallax. [1] It is visible to the naked eye as faint, blue-white hued star with an apparent visual magnitude of 5.16. [2] This object is a member of the Alpha Persei Cluster. [14] [15]

This is a B-type main-sequence star with a stellar classification of B3 V. [3] During the 1930s it was reported to have a variable radial velocity, but that may instead have been due to instrument error. [16] The star has a high rate of spin, showing a projected rotational velocity of 120 km/s. [11] It has 6.8 [7] times the mass of the Sun and about 3.9 [8] times the Sun's radius. 29 Persei is radiating 960 times the Sun's luminosity from its photosphere at an effective temperature of 16,143 K. [6]

Related Research Articles

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

ν Tauri, Latinized as Nu Tauri, is a single star in the zodiac constellation of Taurus. It is a white-hued star and is visible to the naked eye with an apparent visual magnitude of +3.91. This object is located 117 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −6 km/s. It is predicted to come to within roughly 18.4 ly of the Sun in around five million years.

<span class="mw-page-title-main">Eta Tucanae</span> Star in the constellation Tucana

Eta Tucanae, Latinized from η Tucanae, is a probable binary star system in the southern constellation of Tucana, a few degrees to the north of Epsilon Tucanae. It is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude of +5.00. parallax measurements provide a distance estimate of about 154 light years from the Sun, and it is drifting further away with a mean radial velocity of +32.5 km/s. It is a member of the 30 million year old Tucana-Horologium association of co-moving stars.

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

π Persei, Latinized as Pi Persei, is a single star in the northern constellation of Perseus. It has the traditional name Gorgonea Secunda, the second of three Gorgons in the mythology of the hero Perseus. This star has a white hue and is faintly visible to the naked eye with an apparent visual magnitude of +4.7. It is located at a distance of approximately 303 light years from the Sun based on parallax, and is moving further away with a radial velocity of +14 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">Mu Ophiuchi</span> Star in the constellation Ophiuchus

μ Ophiuchi, Latinized as Mu Ophiuchi, is a solitary, blue-white hued star in the equatorial constellation of Ophiuchus. It is visible to the naked as a faint point of light with an apparent visual magnitude of 4.62. This object is located approximately 760 light years away from the Sun based on parallax, but is drifting closer with a radial velocity of −18.5 km/s.

<span class="mw-page-title-main">Epsilon Microscopii</span> Star in the constellation Microscopium

Epsilon Microscopii, Latinized from ε Microscopii, is a single, white-hued star in the southern constellationof Microscopium. It is faintly visible to the naked eye with an apparent visual magnitude of 4.71. The annual parallax shift of the star is 19.7054 mas as measured from Earth, which yields a distance estimate of around 166 light years. It is moving further from the Sun with a radial velocity of +7 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">Epsilon Pavonis</span> Star in the constellation Pavo

Epsilon Pavonis, Latinized from ε Pavonis, is a single, white-hued star in the constellation Pavo. It can be viewed with the naked eye, having an apparent visual magnitude of 3.97. The annual parallax shift of 31.04 mas provides a distance estimate of 105 light years from the Sun. This star is a member of the proposed Argus Association, a young moving group of more than 60 stars associated with the IC 2391 cluster. Epsilon Pavonis is moving closer to the Sun with a radial velocity of −6.7 km/s.

Phi<sup>1</sup> Pavonis Single star in the constellation Pavo

Phi1 Pavonis, latinized from φ1 Pavonis, is a single star in the southern constellation of Pavo. It has a yellow-white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.75. The star is located at a distance of approximately 92 light years away based on parallax. It is drifting closer to the Sun with a radial velocity of −20 km/s.

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

Rho Pegasi, Latinized from ρ Pegasi, is a star in the northern constellation of Pegasus, near the southern constellation boundary with Pisces. This is a probable astrometric binary system, as determined by changes to the proper motion of the visible component. It has a white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.90. The system is located at a distance of approximately 274 light years from the Sun based on parallax, but it is drifting closer with a radial velocity of −10.6 km/s.

<span class="mw-page-title-main">34 Persei</span> Binary star system in the constellation Perseus

34 Persei is a binary star system in the northern constellation of Perseus. It is visible to the naked eye as a faint, blue-white hued point of light with a combined apparent visual magnitude of 4.67. The system is located approximately 540 light years away from the Sun based on parallax, but it is drifting closer with a radial velocity of −3.5 km/s. It is a likely member of the Alpha Persei Cluster.

<span class="mw-page-title-main">54 Persei</span> Star in the constellation Perseus

54 Persei is a single star in the northern constellation of Perseus. It is visible to the naked eye as a faint, yellow-hued star with an apparent visual magnitude of 4.93. The star is located approximately 220 light years away based on parallax, but is drifting closer with a radial velocity of −27 km/s.

<span class="mw-page-title-main">32 Persei</span> Star in the constellation Perseus

32 Persei is a single star located 149 light years away from the Sun in the northern constellation of Perseus. It has the Bayer designation of l Persei, while 32 Persei is the Flamsteed designation. This object is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 4.96. It is moving closer to the Earth with a heliocentric radial velocity of −9 km/s, and is a member of the Sirius supercluster: a stream of stars that share a common motion through space.

<span class="mw-page-title-main">4 Persei</span> Star in the constellation Perseus

4 Persei is a single star in the northern constellation of Perseus, located around 670 light years away from the Sun. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 5.04 The Bayer designation for this star is g Persei; 4 Persei is the Flamsteed designation. This object has a peculiar velocity of 26.3 km/s and may be a runaway star.

<span class="mw-page-title-main">HD 21278</span> Binary star system in the constellation Perseus

HD 21278 is a binary star system in the constellation Perseus, located within the 60±7 million year old Alpha Persei Cluster. It has a blue-white hue and is visible to the naked eye with a combined apparent visual magnitude of 4.99. The system is located at a distance of approximately 580 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +1.20 km/s.

<span class="mw-page-title-main">42 Persei</span> Binary star system in the constellation Perseus

42 Persei is a binary star system in the northern constellation of Perseus. It has the Bayer designation n Persei, while 42 Persei is the Flamsteed designation. The system is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude of 5.11. It is located around 93 parsecs (302 ly) distant from the Sun, but is drifting closer with a radial velocity of −12.4 km/s.

<span class="mw-page-title-main">43 Persei</span> Spectroscopic binary star system in the constellation Perseus

43 Persei is a binary star system in the northern constellation Perseus. It is visible to the naked eye as a dim, yellow-white hued star with an apparent visual magnitude of 5.28. The system is located around 38.5 parsecs (125.4 ly) distant from the Sun, based on parallax.

<span class="mw-page-title-main">31 Persei</span> Star in the constellation Perseus

31 Persei is a single star in the northern constellation of Perseus. It is visible to the naked eye as a dim, blue-white hued point of light with an apparent visual magnitude of 5.05. This star is located around 172 parsecs (560 ly) away from the Sun, and it is drifting closer with a radial velocity of −1.6 km/s. It is likely a member of the Alpha Persei Cluster.

<span class="mw-page-title-main">21 Persei</span> Star in the constellation Perseus

21 Persei is a single, variable star in the northern constellation of Perseus, located about 331 light years away from the Sun. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 5.10 km/s. The object is moving further from the Earth with a heliocentric radial velocity of +8.5 km/s. It has the variable star designation LT Persei; 21 Persei is the Flamsteed designation.

<span class="mw-page-title-main">HD 21071</span> Star in the constellation Perseus

HD 21071 is a blue-white hued variable star in the northern constellation of Perseus. Also known as V576 Persei, it is a sixth magnitude star that is dimly visible to the naked eye under good viewing conditions, having an apparent visual magnitude of 6.09. The brightness of the star varies with a multiperiodic cycle. The distance to HD 21071, as determined from an annual parallax shift of 6.1 mas, is 535 light years. It is a member of the young Alpha Persei cluster, Melotte 20, and moving is closer to the Earth with a heliocentric radial velocity of −1.5 km/s.

References

  1. 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.
  2. 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
  3. 1 2 Hoffleit, D.; Warren, W. H. (1995). "VizieR Online Data Catalog: Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)". VizieR On-line Data Catalog: V/50. Originally Published in: 1964BS....C......0H. 5050. Bibcode:1995yCat.5050....0H.
  4. 1 2 Mallama, A. (2014). "Sloan Magnitudes for the Brightest Stars". The Journal of the American Association of Variable Star Observers. 42 (2): 443. Bibcode:2014JAVSO..42..443M. Vizier catalog entry
  5. Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID   119231169.
  6. 1 2 3 4 Silaj, J.; Landstreet, J. D. (2014). "Accurate age determinations of several nearby open clusters containing magnetic Ap stars". Astronomy & Astrophysics. 566: A132. arXiv: 1407.4531 . Bibcode:2014A&A...566A.132S. doi:10.1051/0004-6361/201321468. S2CID   53370832.
  7. 1 2 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
  8. 1 2 Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics, 367 (Third ed.): 521–524, arXiv: astro-ph/0012289 , Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID   425754.
  9. David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv: 1501.03154 , Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID   33401607.
  10. Gontcharov, G. A. (2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters. 38 (12): 771–782. arXiv: 1606.08814 . Bibcode:2012AstL...38..771G. doi:10.1134/S1063773712120031. S2CID   118345778. Vizier catalog entry
  11. 1 2 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 .
  12. "11 Per". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-03-28.
  13. 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.
  14. Eggen, Olin J. (October 1998), "The Pleiades and alpha Persei Clusters", The Astronomical Journal, 116 (4): 1810–1815, Bibcode:1998AJ....116.1810E, doi: 10.1086/300533
  15. Zuckerman, B.; et al. (June 2012), "Stellar Membership and Dusty Debris Disks in the α Persei Cluster", The Astrophysical Journal, 752 (1): 12, arXiv: 1204.3950 , Bibcode:2012ApJ...752...58Z, doi:10.1088/0004-637X/752/1/58, S2CID   119207634, 58.
  16. Pesch, Peter (June 1967), "Radial Velocities and Spectral Types of Some Bright Blue Stars in the Old Open Cluster M67", Astrophysical Journal, 148: 781, Bibcode:1967ApJ...148..781P, doi: 10.1086/149201