HD 16754

Last updated
HD 16754
Observation data
Epoch J2000       Equinox J2000
Constellation Eridanus
Right ascension 02h 39m 47.96544s [1]
Declination −42° 53′ 30.3638″ [1]
Apparent magnitude  (V)+4.74 [2]
Characteristics
Spectral type A1 Vb [3] + M2-5V [4] + ?
B−V color index 0.061±0.003 [2]
Astrometry
Radial velocity (Rv)+18.0±4.2 [2]  km/s
Proper motion (μ)RA: +88.20 [5]   mas/yr
Dec.: −17.82 [5]   mas/yr
Parallax (π)24.7076 ± 0.3930 [1]   mas
Distance 132 ± 2  ly
(40.5 ± 0.6  pc)
Absolute magnitude  (MV)+1.76 [6]
Details
Aa
Mass 1.95 [7]   M☉
Radius 1.93 [8]   R☉
Luminosity 17.44 [2]   L☉
Surface gravity (log g)4.40±0.14 [7]   cgs
Temperature 9,099±309 [7]   K
Metallicity [Fe/H]−0.06 [3]   dex
Rotational velocity (v sin i)167.6±1.7 [9] or 13.4±1.5 [6]  km/s
Age 212 [7] or 30 [8]   Myr
Other designations
s Eri, CD−43°814, FK5  2185, HD  16754, HIP  12413, HR  789, SAO  215996 [10]
Database references
SIMBAD data

HD 16754 is a binary [11] or triple-star [8] system in the constellation Eridanus. It has the Bayer designation s Eridani; HD 16754 is the designation from the Henry Draper catalogue . The system is visible to the naked eye as a faint point of light with an apparent visual magnitude of +4.74. [2] It is located at a distance of approximately 132  light years from the Sun based on parallax, [1] and is drifting further away with a radial velocity of +18 km/s. [2] The system is a member of the Columba association of co-moving stars. [12]

This object was flagged as an astrometric binary based on proper motion measurements made from the Hipparcos spacecraft. [13] [14] Zuckerman et al. (2011) consider it a multi-star system, with a bright A-type primary plus a faint M-type companion at an angular separation of 25″ to the north. The astrometric companion to the primary remains unresolved. [8]

The main component is an A-type main-sequence star with a stellar classification of A1 Vb. [3] Based upon stellar models, it has an age estimated at 212 million years. [7] Consistency with its membership in the Columba association suggests a much younger age of 30 million years. [8] Earlier measurements showed a high projected rotational velocity of 168 km/s. [9] However, Ammler-von Eiff and Reiners (2012) found a much lower velocity of 13 km/s. [6]

The visible companion is a red dwarf star with a class in the range M2-5V. The system is a source of X-ray emission with a luminosity of 924×1020  W , which is most likely coming from this component and the unresolved companion. [4]

Related Research Articles

Sigma Aquarii Star in the constellation Aquarius

Sigma Aquarii, Latinized from σ Aquarii, is a double star in the equatorial constellation of Aquarius, positioned about 1.3° to the south of the ecliptic. Due to its proximity to the ecliptic, this star is subject to occultation by the Moon. It has a white hue and is visible to the naked eye with an apparent visual magnitude of 4.81. Based upon parallax measurements, the distance to this star is approximately 175 light-years. It is drifting further away with a radial velocity of +11 km/s.

107 Aquarii is a double star in the equatorial constellation of Aquarius. 107 Aquarii is the Flamsteed designation, although it also bears the Bayer designation i2 Aquarii. The pair have an angular separation of 6.787 arcseconds. They have a combined apparent visual magnitude of +5.305, with individual magnitudes of 5.72 and 6.72. The annual parallax shift is 13.66 milliarcseconds with an 8% margin of error. This indicates the system is at a distance of around 240 light-years from Earth.

20 Cancri is an astrometric binary star system in the constellation Cancer, located about 348 light years away from the Sun. This system has the Bayer designation d1 Cancri; 20 Cancri is the Flamsteed designation. It is just visible to the naked eye under good viewing conditions, appearing as a dim, white-hued star with an apparent visual magnitude of 5.94. The pair are moving further from the Earth with a heliocentric radial velocity of +36 km/s, and are members of the Hyades Supercluster.

28 Cancri is a star system in the zodiac constellation of Cancer. It is a variable star with the designation CX Cancri, and is close to the lower limit of visibility with the naked eye, having a mean apparent visual magnitude of 6.05. The annual parallax shift seen from Earth's orbit is 7.32 mas, which provides a distance estimate of about 450 light years. It is moving away from the Sun with a radial velocity of around +9 km/s.

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).

Delta Columbae is a binary star system in the constellation Columba. It can be seen with the naked eye having an apparent visual magnitude of 3.85. The distance to this system, based upon an annual parallax shift of 13.94 mas, is around 234 lightyears.

5 Tauri is a binary star in the zodiac constellation of Taurus, located approximately 530 light years from the Sun. It is visible to the naked eye as a faint orange-hued star with an apparent visual magnitude of +4.14. It is moving further from the Earth with a heliocentric radial velocity of +14 km/s.

14 Eridani is a star in the equatorial Eridanus constellation. It has an apparent visual magnitude of 6.143 and is moving closer to the Sun with a radial velocity of around −5 km/s. The measured annual parallax shift is 29.26 mas, which provides an estimated distance of about 121 light years. Proper motion studies indicate that this is an astrometric binary.

HD 179791 is suspected variable star in the equatorial constellation of Aquila. It is a challenge to see with the naked eye even under good viewing conditions, having an apparent visual magnitude of 6.48. The distance to HD 179791 can be estimated from its annual parallax shift of 5.3 mas, which yields a value of 616 light years. It is moving further from the Earth with a heliocentric radial velocity of +16 km/s. Astrometric measurements of the star show changes in motion that may indicate it is a member of a close binary system.

HD 15524 is a wide binary star in the northern zodiac constellation of Aries. Located approximately 51.76 parsecs (168.8 ly) away, the primary, a yellow-white subgiant or main sequence star has an apparent magnitude of 5.97, meaning that it can be viewed with the naked eye under good conditions. The secondary, separated from the primary by 12.4 arcseconds, has an apparent magnitude of 10.4.

6 Equulei is a probable astrometric binary star system in the northern constellation of Equuleus, located 380 light years from the Sun. It is barely visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 6.07. The system is moving further away from the Earth with a heliocentric radial velocity of +6.9 km/s. It forms a wide optical double with γ Equulei, at an angular separation of 336 arcseconds in 2011.

HD 114837 is a suspected binary star system in the southern constellation of Centaurus. The brighter star is faintly visible to the naked eye with an apparent visual magnitude of 4.90. It has a magnitude 10.2 candidate common proper motion companion at an angular separation of 4.2″, as of 2014. The distance to this system, based on an annual parallax shift of 55.0143″ as seen from Earth's orbit, is 59.3 light years. It is moving closer with a heliocentric radial velocity of −64 km/s, and will approach to within 21.8 ly in around 240,600 years.

HD 83446 is a probable astrometric binary star system in the constellation Vela. It is visible to the naked eye with an apparent visual magnitude of 4.34. Based upon an annual parallax shift of 30.5 mas, it is located 107.1 light years from the Sun. The system is moving further away with a heliocentric radial velocity of +18 km/s.

Xi<sup>1</sup> Lupi

Xi1 Lupi (ξ1 Lup, ξ1 Lupi) is a probable binary star in the southern constellation of Lupus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.1, and forms a visual double star with Xi2 Lupi. Based upon an annual parallax shift of 23.60 mas as seen from Earth, it is located around 140 light years from the Sun. It is a member of the Upper Scorpius sub-group of the nearby Sco OB2 association.

59 Persei is a suspected astrometric binary star system in the northern constellation of Perseus. It is visible to the naked eye as a dim, white-hued star with an apparent magnitude of 5.30. The star is located around 256 light years distant from the Sun, based on parallax, and is drifting further away with a radial velocity of +13 km/s.

55 Persei Star in the constellation Perseus

55 Persei is a single, blue-white hued star in the northern constellation Perseus. It is faintly visible to the naked eye under good seeing conditions, having an apparent visual magnitude of 5.73. Based upon an annual parallax shift of 8.50±0.38 mas as seen from Earth's orbit, the star is located about 380 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction of 0.39 due to interstellar dust.

74 Cygni is a visual binary star system in the northern constellation Cygnus, located around 249 light years distant from the Sun. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.04. The pair orbit each other with a period of 1.57 years and an eccentricity of 0.5. The system is a source of X-ray emission, which is most likely coming from the secondary component.

53 Ophiuchi is a multiple star system in the equatorial constellation of Ophiuchus. It is visible to the naked eye as a faint star with a combined apparent visual magnitude of 5.80. Located around 370 light years distant from the Sun based on parallax, it is moving closer to the Earth with a heliocentric radial velocity of −14 km/s. As of 2011, the visible components had an angular separation of 41.28″ along a position angle of 190°. The primary may itself be a close binary system with a separation of 0.3692″ and a magnitude difference of 3.97 at an infrared wavelength of 562 nm.

ε Fornacis is the Bayer designation for a high proper motion binary star in the southern constellation of Fornax. It is faintly visible to the naked eye with an apparent visual magnitude of 5.89. Based upon an annual parallax shift of 31.06 mas, the system is located roughly 105 light years from the Sun. At that distance, its visual magnitude is reduced by an interstellar absorption factor of 0.09 due to dust.

HD 111456 is a yellow-white hued star in the northern circumpolar constellation of Ursa Major. It is dimly visible to the naked eye, having an apparent visual magnitude of 5.85. Based upon an annual parallax shift of 38.2 mas as seen from Earth, it is located about 85 light years from the Sun. The star is moving closer to the Sun with a radial velocity of −18 km/s. HD 111456 is a nucleus cluster member of the Ursa Major Moving Group, a set of stars that are moving through space with a similar heading and velocity. Six other stars in the nucleus of the group are prominent members of the Big Dipper asterism.

References

  1. 1 2 3 4 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 5 6 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 Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal , 132 (1): 161–170, arXiv: astro-ph/0603770 , Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID   119476992.
  4. 1 2 Schröder, C.; Schmitt, J. H. M. M. (November 2007), "X-ray emission from A-type stars", Astronomy and Astrophysics, 475 (2): 677–684, Bibcode:2007A&A...475..677S, doi: 10.1051/0004-6361:20077429 .
  5. 1 2 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.
  6. 1 2 3 Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: A116, arXiv: 1204.2459 , Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, S2CID   53666672.
  7. 1 2 3 4 5 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.
  8. 1 2 3 4 5 Zuckerman, B.; et al. (May 2011), "The Tucana/Horologium, Columba, AB Doradus, and Argus Associations: New Members and Dusty Debris Disks", The Astrophysical Journal, 732 (2): 61, arXiv: 1104.0284v1 , Bibcode:2011ApJ...732...61Z, doi:10.1088/0004-637X/732/2/61, S2CID   62797470.
  9. 1 2 Díaz, C. G.; et al. (July 2011), "Accurate stellar rotational velocities using the Fourier transform of the cross correlation maximum", Astronomy & Astrophysics, 531: A143, arXiv: 1012.4858 , Bibcode:2011A&A...531A.143D, doi:10.1051/0004-6361/201016386, S2CID   119286673.
  10. ↑ "HD 16754". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-12-16.
  11. ↑ 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.
  12. ↑ Elliott, P.; et al. (May 2016), "Search for associations containing young stars (SACY). VII. New stellar and substellar candidate members in the young associations", Astronomy & Astrophysics, 590: 28, arXiv: 1604.03550 , Bibcode:2016A&A...590A..13E, doi:10.1051/0004-6361/201628253, S2CID   53138126, A13.
  13. ↑ Makarov, V. V.; Kaplan, G. H. (May 2005), "Statistical Constraints for Astrometric Binaries with Nonlinear Motion", The Astronomical Journal, 129 (5): 2420–2427, Bibcode:2005AJ....129.2420M, doi: 10.1086/429590 .
  14. ↑ Frankowski, A.; et al. (March 2007), "Proper-motion binaries in the Hipparcos catalogue. Comparison with radial velocity data", Astronomy and Astrophysics, 464 (1): 377–392, arXiv: astro-ph/0612449 , Bibcode:2007A&A...464..377F, doi:10.1051/0004-6361:20065526, S2CID   14010423.
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.