7 Camelopardalis

Last updated
7 Camelopardalis
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Camelopardalis
Right ascension 04h 57m 17.19609s [1]
Declination +53° 45′ 07.5654″ [1]
Apparent magnitude  (V)4.43 [2] (4.49 + ? + 7.90 + 11.30) [3]
Characteristics
Evolutionary stage main sequence
Spectral type A1 V [4]
B−V color index −0.017±0.003 [2]
Astrometry
Radial velocity (Rv)−9.5±3.7 [5]  km/s
Proper motion (μ)RA: −24.51 [1]   mas/yr
Dec.: +7.71 [1]   mas/yr
Parallax (π)8.77 ± 0.60  mas [1]
Distance 370 ± 30  ly
(114 ± 8  pc)
Absolute magnitude  (MV)−0.84 [2]
Orbit [6]
Primary7 Cam Aa
Companion7 Cam Ab
Period (P)3.884 d
Eccentricity (e)0
Periastron epoch (T)2,457,726.05  JD
Argument of periastron (ω)
(secondary)		0°
Semi-amplitude (K1)
(primary)		34.9±0.2 km/s
Details
7 Cam Aa
Mass 3.16±0.10 [7]   M☉
Luminosity 221.6+36.8
−31.5 [7]   L☉
Temperature 9,226+236
−231 [7]   K
Rotational velocity (v sin i)40 [7]  km/s
Other designations
7 Cam, BD+53°829, GC  6017, HD  31278, HIP  23040, HR  1568, SAO  24929, ADS  3536, WDS J04573+5345 [8]
Database references
SIMBAD data

7 Camelopardalis is a multiple star system [9] in the northern circumpolar constellation of Camelopardalis. It is located approximately 370 light years from the Sun, as determined from its parallax. [1] This system is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 4.43. [2] It is moving closer to the Earth with a heliocentric radial velocity of −10 km/s. [5]

The primary member of the group, designated component A, is a single-lined spectroscopic binary system with a circular orbit and a period of 3.88 days. [6] The visible component of this pair is a magnitude 4.49 [3] A-type main-sequence star with a stellar classification of A1 V. [4] It has 3.2 times the mass of the Sun and is spinning with a projected rotational velocity of 40 km/s. The star is radiating 222 times the Sun's luminosity from its photosphere at an effective temperature of 9,226 K. [7]

The magnitude 7.90 [3] component B has an orbital solution with the Aa/Ab pair, which yields a period of 284 years and an eccentricity of 0.74. However, Drummond (2014) found the data to be discordant and instead determined that they are an optical pair with no physical association. [10] The fourth member, component C, is a magnitude 11.30 star at an angular separation of 25.50″ along a position angle of 242° from the primary, as of 2003. [3] It shares a common proper motion with the primary star. [11]

Related Research Articles

<span class="mw-page-title-main">Gamma Volantis</span> K-type giant star in the constellation Volans

Gamma Volantis, Latinized from γ Volantis, is a wide binary star system in the southern constellation of Volans. Based upon parallax measurements, it is approximately 133 light years from Earth. It is bright enough to be seen with the naked eye and can be found around 9° to the east-southeast of the Large Magellanic Cloud.

<span class="mw-page-title-main">8 Andromedae</span> Mulitple star system in the constellation Andromeda

8 Andromedae, abbreviated 8 And, is a probable triple star system in the northern constellation of Andromeda. 8 Andromedae is the Flamsteed designation. It is visible to the naked eye with an apparent visual magnitude of 4.82. Based upon an annual parallax shift of 5.7 mas, it is located about 570 light years from the Earth. It is moving closer with a heliocentric radial velocity of −8 km/s.

59 Andromedae, abbreviated 59 And, is a sixth-magnitude binary star system in the northern constellation of Andromeda. 59 Andromedae is the Flamsteed designation. As of 2017, the pair had an angular separation of 16.60″ along a position angle (PA) of 36°. Compare this to a separation of 15.3″ along a PA of 35°, as measured in 1783. The two stars have an estimated physical separation of 1,370 AU.

66 Cancri is a binary star system near the northern border of the zodiac constellation of Cancer, located 474 light years away from the Sun. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.87. The pair are moving closer to the Earth with a heliocentric radial velocity of −13 light years. As of 2003, the magnitude 8.56 companion was located at an angular separation of 4.43″ along a position angle of 134° from the primary.

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

Gamma Camelopardalis, Latinized from γ Camelopardalis, is a suspected wide binary star system in the northern circumpolar constellation of Camelopardalis. With a visual magnitude of 4.66, it is faintly visible to the naked eye. Based upon an annual parallax shift of 9.09 mas as seen from Earth, this star is located about 359 light years from the Sun.

<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">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.

HD 225218 is a quadruple star system in the northern constellation of Andromeda. The primary component, HD 225218 A, is a giant star with a stellar classification of B9III, an apparent magnitude of 6.16, and is a candidate Lambda Boötis star. It has a fainter, magnitude 9.65 companion, HD 225218 B, at an angular separation of 5.2″ along a position angle of 171°. The primary itself has been identified as a binary star system through interferometry, with the two components separated by 0.165″. The pair, HD 225218 Aa and Ab, orbit each other with a period of about 70 years and an eccentricity of 0.515. Component B is likewise a spectroscopic binary.

HD 6114 is a visual binary star system in the northern constellation of Andromeda. With a combined apparent magnitude of 6.46, the star can only be seen with the naked eye by keen-eyed observers even on the best of nights. Based upon an annual parallax shift of 10.4 mas as seen from Earth's orbit, the system is located approximately 108 parsecs (350 ly) distant.

HD 152010 is a solitary star in the southern circumpolar constellation Apus. It has an apparent magnitude of 6.48, placing it near the max visibility for the naked eye. Located 1,006 light yearsaway, the object is approaching the Solar System with a heliocentric radial velocity of −15 km/s.

4 Camelopardalis is a probable multiple star in the northern constellation of Camelopardalis, located 177 light years away from the Sun, based upon parallax. With a combined apparent visual magnitude of 5.29, it is visible to the naked eye as a faint, white-hued star. The pair have a relatively high proper motion, traversing the celestial sphere at an angular rate of 0.158″ per year. The system's proper motion makes it a candidate for membership in the IC 2391 supercluster. They are moving away from the Earth with a heliocentric radial velocity of 22.5 km/s.

HD 3 is a single, white-hued star in the northern constellation Andromeda. With an apparent visual magnitude of 6.71, it is below the nominal brightness limit for visibility with the typical naked eye but may still be visible by some observers under ideal viewing conditions. It is also the first star indexed in the Bright Star Catalogue. Based upon an annual parallax shift of 6.3137±0.0826 mas, it is located roughly 517 light years away. The star is moving closer with a heliocentric radial velocity of −18 km/s, and will make perihelion in around 2.9 million years at a separation of around 351 ly (107.71 pc).

<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.

Tau1 Hydrae is a triple star system in the equatorial constellation of Hydra. Based upon the annual parallax shift of the two visible components as seen from Earth, they are located about 18 parsecs (59 ly) from the Sun. The system has a combined apparent visual magnitude of +4.59, which is bright enough to be visible to the naked eye at night.

HD 44120 is a wide binary star system in the southern constellation of Pictor. Although visible to the naked eye, it is a challenge to view having an apparent visual magnitude of 6.44. The system is located at a distance of 118 light years from the Sun based on parallax, but it is drifting closer with a radial velocity of −2 km/s. It has an absolute magnitude of 3.57.

HD 179886 is a binary star located in the southern constellation Telescopium. It has a combined apparent magnitude of 5.37, making it faintly visible to the naked eye if viewed under ideal conditions. The system is situated at a distance of 700 light years but is receding with a heliocentric radial velocity of 6.3 km/s.

HD 20104 is a visual binary in the northern circumpolar constellation Camelopardalis. The system has a combined apparent magnitude of 6.41, making it near naked eye visibility. When resolved in a large telescope, HD 20104 appears to be a pair of 7th magnitude A-type main-sequence stars with a separation of about 0.5″. Located approximately 550 light years away, the system is approaching the Sun with a heliocentric radial velocity of −6 km/s.

13 Delphini is a binary star in the equatorial constellation Delphinus, with a combined apparent magnitude of 5.64. The system is located at a distance of 471 light years but is approaching the Solar System with a heliocentric radial velocity of about −7 km/s.

HD 182509, also designated as HR 7370, is an orange hued star located in the southern constellation Telescopium. It has an apparent magnitude of 5.69, making it faintly visible to the naked eye if viewed under ideal conditions. Parallax measurements place the object at a distance of 635 light years. It has a poorly constrained heliocentric radial velocity of −5 km/s, indicating that it is drifting towards the Solar System.

HD 208741, also known as HR 8380, is a yellowish-white hued star located in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.91, making it faintly visible to the naked eye. Parallax measurements place it at a distance of 211 light years, and it is currently receding with a heliocentric radial velocity of 8 km/s.

References

  1. 1 2 3 4 5 6 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv: 0708.1752 , Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID   18759600.
  2. 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.
  3. 1 2 3 4 Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode:2001AJ....122.3466M, doi: 10.1086/323920 .
  4. 1 2 Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819.
  5. 1 2 de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv: 1208.3048 , Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID   59451347, A61.
  6. 1 2 Heyne, T.; Mugrauer, M.; Bischoff, R.; Wagner, D.; Hoffmann, S.; Lux, O.; Munz, V.; Geymeier, M.; Neuhäuser, R. (2020). "Spectroscopic characterization of nine binary star systems as well as HIP 107136 and HIP 107533". Astronomische Nachrichten. 341 (1): 99–117. arXiv: 1912.05343 . Bibcode:2020AN....341...99H. doi:10.1002/asna.202013683. S2CID   209202812.
  7. 1 2 3 4 5 Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv: 1201.2052 , Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID   55586789.
  8. ↑ "7 Cam". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-04-15.
  9. ↑ Eggleton, P. P.; et al. (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.
  10. ↑ Drummond, Jack D. (March 2014), "Binary Stars Observed with Adaptive Optics at the Starfire Optical Range", The Astronomical Journal, 147 (3): 10, Bibcode:2014AJ....147...65D, doi: 10.1088/0004-6256/147/3/65 , 65.
  11. ↑ 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.
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.