44 Andromedae

Last updated
44 Andromedae
Observation data
Epoch J2000.0       Equinox J2000.0 (ICRS)
Constellation Andromeda
Right ascension 01h 10m 18.74041s [1]
Declination +42° 04′ 53.3100″ [1]
Apparent magnitude  (V)5.67 [2]
Characteristics
Spectral type F8 V [3]
U−B color index +0.12 [2]
B−V color index +0.59 [2]
Astrometry
Radial velocity (Rv)−14.2±0.2 [4]  km/s
Proper motion (μ)RA: −135.569(38) [1]   mas/yr
Dec.: −41.790(30) [1]   mas/yr
Parallax (π)18.8145 ± 0.0376  mas [1]
Distance 173.4 ± 0.3  ly
(53.2 ± 0.1  pc)
Absolute magnitude  (MV)+2.07 [5]
Details [3]
Mass 1.64  M☉
Radius 3.58±0.19  R☉
Luminosity 12.9  L☉
Surface gravity (log g)3.78±0.07  cgs
Temperature 6,028±32  K
Metallicity [Fe/H]−0.01±0.04  dex
Rotation 15.2 d
Rotational velocity (v sin i)11.6±0.8 km/s
Age 2.59  Gyr
Other designations
44 And, BD+41° 219, FK5  2075, GC  1410, GJ  53.4, HD  6920, HIP  5493, HR  340, SAO  36984, PPM  43709 [6]
Database references
SIMBAD data

44 Andromedae is a single, [7] yellow-white hued star in the northern constellation of Andromeda. [6] 44 Andromedae is the Flamsteed designation. It has an apparent visual magnitude of approximately 5.67, [2] which indicates it is a dim star that is just visible to the naked eye on a dark night. The annual parallax shift as measured by the Hipparcos spacecraft is 18.8145  mas, [1] which yields a distance estimate of around 173  light years. It is moving closer to the Sun with a radial velocity of −14 km/s. [4]

This star has been assigned a stellar classification of F8 V, [3] which indicates it is an ordinary F-type main-sequence star. However, Gray et al. (2001) gave it a class of F9 IV, suggesting it is instead a subgiant star that is evolving away from the main sequence as the hydrogen fuel at its core becomes exhausted. [8] It is an estimated 2.6 billion years old and is rotating with a period of 15.2 days. The star has 1.64 times the mass of the Sun and 3.6 times the Sun's radius. It is radiating 13 times the Sun's luminosity from its photosphere at an effective temperature of 6,028 K. [3] It appears overluminous for a star of its type which may indicate the presence of a bright companion, but no radial velocity variation has been detected. [9]

Related Research Articles

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

Pi Andromedae is the Bayer designation for a binary star system in the northern constellation of Andromeda. With an apparent visual magnitude of 4.4, it is visible to the naked eye. It is located approximately 580 light-years from Earth.

<span class="mw-page-title-main">Theta Andromedae</span> Binary star in the constellation Andromeda

Theta Andromedae is a binary star system in the northern constellation of Andromeda. Theta Andromedae, Latinized from θ Andromedae, is its Bayer designation. It is located at a distance of approximately 173 light-years from the Sun, and has an apparent visual magnitude of 4.6. On the Bortle Dark-Sky Scale, this makes it visible to the naked eye from outside urban regions. Based on its motion through space, this system appears to be a member of the Sirius supercluster.

<span class="mw-page-title-main">Xi Andromedae</span> K-type giant star in the constellation Andromeda

Xi Andromedae, officially named Adhil, is a solitary star in the northern constellation of Andromeda. It has an apparent magnitude of +4.9. Based on parallax measurements obtained during the Gaia mission, it lies at a distance of roughly 223 light-years from the Sun.

<span class="mw-page-title-main">Chi Andromedae</span> Star in the constellation Andromeda

Chi Andromedae is the Bayer designation for a star in the northern constellation of Andromeda. It has an apparent visual magnitude of +5.01, which is relatively faint for a naked-eye star. Based upon parallax measurements made during the Gaia mission, Chi Andromedae is located around 264 light-years from Earth.

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

Rho Andromedae, Latinized from ρ Andromedae, is the Bayer designation for a star in the northern constellation of Andromeda. It has an apparent visual magnitude of +5.19, which, according to the Bortle Dark-Sky Scale, is bright enough to be seen with the naked eye from dark suburban skies. Based upon parallax measurements, this star is at a distance of approximately 162 light-years from the Sun. It is drifting further away with a radial velocity of +10 km/s.

22 Andromedae, abbreviated 22 And, is a single star in the constellation Andromeda. 22 Andromedae is the Flamsteed designation. It is visible to the naked eye with an apparent visual magnitude of 5.04. The distance to 22 And can be estimated from its annual parallax shift of just 2.2 mas, which shows it to be around 1,500 light years away. It is moving closer to the Earth with a heliocentric radial velocity of −8.2 km/s.

41 Andromedae is a single star in the northern constellation of Andromeda. 41 Andromedae is the Flamsteed designation. It is bright enough to be faintly visible to the naked eye, having an apparent visual magnitude of 5.04. Based upon an annual parallax shift of 16.4 mas, it is located 198 light years away. The star is moving further from the Earth with a heliocentric radial velocity of +10 km/s and it has a relatively high rate of proper motion, traversing the celestial sphere at the rate of 0.171″ per year.

5 Andromedae is a single, yellow-white hued star in the northern constellation of Andromeda. Its designation comes from a catalogue of stars by English astronomer John Flamsteed, published in 1712. The star is faintly visible to the naked eye, having an apparent visual magnitude of 5.68. Based upon an annual parallax shift of 29.12 mas as seen from Earth, it is located 112 light years away. 5 Andromedae is moving closer to the Sun with a radial velocity of −2.6 km/s. It has a relatively high proper motion, advancing across the celestial sphere at the rate of 0.201 arc seconds per year.

12 Andromedae is a single star in the northern constellation of Andromeda. The designation is from the star catalogue of English astronomer John Flamsteed, first published in 1712. It has an apparent visual magnitude of 5.87, which indicates it is just visible to the naked eye under good seeing conditions. An annual parallax shift of 23.7806 mas provides a distance estimate of 137 light years. The star is moving closer to the Sun with a radial velocity of −10.5 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.

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

<span class="mw-page-title-main">LN Andromedae</span> Star in the constellation Andromeda

LN Andromedae, also known as HD 217811, HR 8768, is a formerly suspected variable star in the constellation Andromeda. Located approximately 458 parsecs (1,490 ly) away from Earth, it shines with an apparent visual magnitude 6.41, thus it can be seen by the naked eye under very favourable conditions. Its spectral classification is B2V, meaning that it's a hot main sequence star, emitting light approximately with a blackbody spectrum at an effective temperature of 18,090 K.

HD 130458 is a double star in the southern circumpolar constellation of Apus. The pair has a combined apparent magnitude of 5.8, making it faintly visible to the naked eye under ideal conditions. Parallax measurements place the system 310-24 light years away and it is receding with a heliocentric radial velocity of 31.4 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.

<span class="mw-page-title-main">32 Tauri</span> Yellow-white hued subgiant star in the constellation Taurus.

32 Tauri is the Flamsteed designation for a solitary star in the zodiac constellation of Taurus. It has a visual magnitude of 5.64, making it visible to the naked eye from suburban skies. The position of this star near the ecliptic plane means that it is subject to occultations by the Moon. Parallax measurements put it at a distance of 144 light years from the Sun. It is drifting further away with a radial velocity of +31.9 km/s, having come to within 88.9 light-years some 759,000 years ago.

MT Pegasi is a single, yellow-hued star in the northern constellation of Pegasus. It has the designation HD 217813 in the Henry Draper Catalogue; MT Pegasi is the variable star designation. With an apparent visual magnitude of 6.616, it is a dim star that is at or below the nominal limit for visibility with the naked eye. Based upon an annual parallax shift of 41.16 mas as measured from Earth's orbit, it is located 79.24 light years away. This star is a member of the Ursa Major Moving Group, a collection of stars that originated in the same open cluster and now share a common motion through space.

<span class="mw-page-title-main">HD 25291</span> Star in the constellation Camelopardalis

HD 25291, also known as HR 1242, is a solitary, yellowish-white hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.12, making it one of the brighter members of this generally faint constellation. The object is relatively far at a distant of approximately 2,100 light years but is drifting closer with a heliocentric radial velocity of −20.3 km/s.

<span class="mw-page-title-main">Tau Octantis</span> Star in the southern constellation of Octans

Tau Octantis, Latinized from τ Octantis, is a solitary star in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.50, allowing it to be faintly seen with the naked eye. The object is located at a distance of 480 light years but is receding with a heliocentric radial velocity of 31 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 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 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 Guetter, H. H.; Hewitt, A. V. (June 1984), "Photoelectric UBV photometry for 317 PZT and VZT stars", Publications of the Astronomical Society of the Pacific, 96: 441–443, Bibcode:1984PASP...96..441G, doi: 10.1086/131362 .
  3. 1 2 3 4 Marsden, S. C.; et al. (November 2014), "A BCool magnetic snapshot survey of solar-type stars", Monthly Notices of the Royal Astronomical Society, 444 (4): 3517–3536, arXiv: 1311.3374 , Bibcode:2014MNRAS.444.3517M, doi:10.1093/mnras/stu1663, S2CID   53988884.
  4. 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.
  5. ↑ HD 6920, database entry, The Geneva-Copenhagen Survey of Solar neighbourhood, J. Holmberg et al., 2007, CDS ID V/117A. Accessed on line November 19, 2008.
  6. 1 2 "44 And". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2017-12-28.
  7. ↑ 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.
  8. ↑ Gray, R. O.; Napier, M. G.; Winkler, L. I. (April 2001), "The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. I. Precise Spectral Types for 372 Stars", The Astronomical Journal, 121 (4): 2148–2158, Bibcode:2001AJ....121.2148G, doi:10.1086/319956.
  9. ↑ Griffin, R. F.; Suchkov, A. A. (July 2003), "The Nature of Overluminous F Stars Observed in a Radial-Velocity Survey", The Astrophysical Journal Supplement Series, 147 (1): 103–144, Bibcode:2003ApJS..147..103G, doi: 10.1086/367855 .
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