HD 211575

Last updated
HD 211575
HD 211575.png
The region around HD 211575
Observation data
Epoch J2000       Equinox J2000
Constellation Aquarius
Right ascension  22h 18m 04.2722s [1]
Declination −00° 14′ 15.557″ [1]
Apparent magnitude  (V)6.40 [2]
Characteristics
Spectral type F3 V [3]
B−V color index 0.441±0.003 [4]
Astrometry
Radial velocity (Rv)+14.8±0.5 [5]  km/s
Proper motion (μ)RA: −41.997 [1]   mas/yr
Dec.: +54.407 [1]   mas/yr
Parallax (π)24.13 ± 0.29 [6]   mas
Distance 135 ± 2  ly
(41.4 ± 0.5  pc)
Absolute magnitude  (MV)3.31 [2]
Details
Mass 1.27 [7]   M☉
Luminosity 4.30 [4]   L☉
Surface gravity (log g)4.15 [2]   cgs
Temperature 6,574±224 [7]   K
Metallicity [Fe/H]+0.11±0.11 [5]   dex
Rotational velocity (v sin i)19.0 [2]  km/s
Age 150 [5]   Myr
Other designations
BD−00° 4333, HD  203222, HIP  110091, HR  8507, SAO  146004 [8]
Database references
SIMBAD data

HD 211575 is a star in the constellation Aquarius in between "Gamma Aquarii", "Pi Aquarii" and "Sadalmelik". It is a member of the corona of the Ursa Major moving group. [9]

Related Research Articles

Delta Aquarii Star in the constellation Aquarius

Delta Aquarii, officially named Skat, is the third-brightest star in the constellation of Aquarius. The apparent visual magnitude is 3.3, which can be seen with the naked eye. The distance to this star is about 113 light-years based upon parallax measurements, and it has a close companion.

Kappa1 Sculptoris is a binary star system in the southern constellation of Sculptor. It is faintly visible to the naked eye, with a combined apparent visual magnitude of +5.51. Based upon an annual parallax shift of 12.91 mas as measured from Earth, it is located roughly 250 light years from the Sun.

Tau Virginis star in the constellation Virgo

Tau Virginis is a single star in the zodiac constellation Virgo. With an apparent visual magnitude of 4.28, it is faintly visible to the naked eye. The distance to Tau Virginis, based upon parallax measurements, is approximately 225 light years with a margin of error of ±3 light years.

Iota Aquarii Star in the constellation Aquarius

Iota Aquarii, Latinized from ι Aquarii, is the Bayer designation for a star in the equatorial constellation of Aquarius. It is visible to the naked eye with an apparent magnitude of +4.279. Based upon parallax measurements made during the Hipparcos mission, the distance to this star is around 175 light-years.

99 Aquarii Star in the constellation Aquarius

99 Aquarii is a star in the equatorial constellation of Aquarius. 99 Aquarii is the Flamsteed designation, although it also bears the Bayer designation b2 Aquarii. It is visible to the naked eye with an apparent visual magnitude of 4.38; according to the Bortle Dark-Sky Scale this is bright enough to be seen even from city skies under ideal viewing conditions. Based upon parallax measurements, the distance to this star is around 283 light-years.

32 Aquarii is a binary star system in the zodiac constellation of Aquarius. 32 Aquarii is its Flamsteed designation. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 5.29. This system is moving away from the Earth with a heliocentric radial velocity of +19 km/s, and is a possible member of the corona of the Ursa Major flow.

18 Aquarii is a single, yellow-white hued star in the equatorial constellation of Aquarius. The designation is from the catalogue of English astronomer John Flamsteed, first published in 1712. The star is faintly visible to the naked eye with an apparent visual magnitude of 5.49 and is located about 154 light-years from Earth.

19 Aquarii is a star in the zodiac constellation of Aquarius. With an apparent magnitude of about 5.7, the star is barely visible to the naked eye as a white-hued star. Parallax estimates put it at a distance of about 260 light years away from the Sun. The star is moving closer to the Earth with a heliocentric radial velocity of −21 km/s.

20 Aquarii, abbreviated 20 Aqr, is a star in the constellation Aquarius. 20 Aquarii is the Flamsteed designation. It is a dim star with an apparent visual magnitude of 6.38. Based upon an annual parallax shift of 15.34 mas, it is located 213 light years away but is moving closer to the Earth with a heliocentric radial velocity of −23 km/s. The star is predicted to come to within 110 light-years in around 1.9 million years.

42 Aurigae is a star in the northern constellation of Auriga. The designation is from the star catalogue of English astronomer John Flamsteed, first published in 1712. It has an apparent visual magnitude of 6.53, which places it just below the visibility limit for normal eyesight under good seeing conditions. It displays an annual parallax shift of 13.24 mas, which yields a distance estimate of around 246 light years. The star is moving closer to the Sun with a radial velocity of −12 km/s. It is a member of the Ursa Major Moving Group of stars that share a common motion through space.

Nu Caeli is a yellow-white hued star in the constellation Caelum. It has an apparent visual magnitude of 6.07, which indicates it is near the lower limit on brightness that is visible to the naked eye. According to the Bortle scale, the star can be viewed from dark suburban skies. Based upon an annual parallax shift of 19.03 mas as seen from Earth, this star is located about 171 light years from the Sun.

HD 42818 is a suspected astrometric binary star system in the northern circumpolar constellation of Camelopardalis. It is visible to the naked eye with an apparent visual magnitude of +4.76. Based upon an annual parallax shift of 18.64±0.23 mas as seen from Earth's orbit, it is located some 175 light years away. The system appears to be moving closer with a heliocentric radial velocity of −7 km/s. As of 2012, it is estimated that the system will make its closest approach to the Sun in 485,000 years at a distance of around 169.2 ly (51.87 pc).

Pi Cassiopeiae Variable star in the constellation Cassiopeia

Pi Cassiopeiae, Latinized from π Cassiopeiae, is a close binary star system in the constellation Cassiopeia. It is visible to the naked eye with an apparent visual magnitude of +4.949. Based upon an annual parallax shift of 18.63 mas as seen from Earth, this system is located about 175 light years from the Sun.

HD 21447 is a probable binary star system located in the constellation Camelopardalis. The star is also known as HR 1046. It can be viewed with the naked eye, having an apparent visual magnitude of 5.09. Based upon an annual parallax shift of 16.42±0.29 mas, it is located some 199 light years from the Sun. It is a candidate for membership in the Ursa Major Moving Group.

HD 93194 star

HD 93194 is a star in the constellation Carina. Its apparent magnitude is 4.79. Its parent cluster is IC 2602.

HD 93607 star

HD 93607 is a star in the constellation Carina. Its apparent magnitude is 4.87. Its parent cluster is IC 2602.

Lambda Coronae Borealis star in the constellation Corona Borealis

Lambda Coronae Borealis, Latinised from λ Coronae Borealis, is a star located in the constellation Corona Borealis, at a distance of 41.6 parsecs (136 ly). It is also known as HR 5936, and HD 142908.

16 Librae is a star in the constellation Libra. It is a faint star but visible to the naked eye with an apparent visual magnitude of 4.49. An annual parallax shift of 37.17 mas yields a distance estimate of 87.7 light years. It is moving further from the Sun with a radial velocity of +26 km/s.

Beta Pavonis star in the constellation Pavo

Beta Pavonis, Latinized from β Pavonis, is a single, white-hued star in the southern constellation of Pavo. It can be seen with the naked eye, having an apparent visual magnitude of 3.42. Based upon an annual parallax shift of 24.14 mas as seen from Earth, it is located 135 light years from the Sun. It is moving away from the Sun with a radial velocity of +4 km/s. Beta Pavonis is a member of the Ursa Major Moving Group, a set of stars that share a similar motion through space.

Sigma2 Gruis is a binary star system in the southern constellation of Grus. Its apparent visual magnitude is 5.86. The pair had an angular separation of 2.7 arc seconds along a position angle of 265°, as of 1991. Located around 215 ly (66 pc) distant, the white-hued primary component is an A-type main-sequence star of spectral type A1V, a star that is currently fusing its core hydrogen.

References

  1. 1 2 3 4 Brown, A. G. A.; et al. (2016), "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties", Astronomy and Astrophysics, 595, A2, arXiv: 1609.04172 , Bibcode:2016A&A...595A...2G, doi:10.1051/0004-6361/201629512.
  2. 1 2 3 4 Paunzen, E.; et al. (July 2014), "Investigating the possible connection between λ Bootis stars and intermediate Population II type stars", Astronomy & Astrophysics, 567: 8, arXiv: 1406.3936 , Bibcode:2014A&A...567A..67P, doi:10.1051/0004-6361/201423817, A67.
  3. ↑ Houk, N.; Swift, C. (1999), "Michigan catalogue of two-dimensional spectral types for the HD Stars", Michigan Spectral Survey, 5, Bibcode:1999MSS...C05....0H.
  4. 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.
  5. 1 2 3 Casagrande, L.; et al. (2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", Astronomy & Astrophysics, 530 (A138): 21, arXiv: 1103.4651 , Bibcode:2011A&A...530A.138C, doi:10.1051/0004-6361/201016276.
  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.
  7. 1 2 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.
  8. ↑ "HD 211575". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2018-05-11.
  9. ↑ Chupina, N. V.; et al. (June 2006), "Kinematic structure of the corona of the Ursa Major flow found using proper motions and radial velocities of single stars", Astronomy and Astrophysics, 451 (3): 909−916, Bibcode:2006A&A...451..909C, doi: 10.1051/0004-6361:20054009 .
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