Rho1 Arae

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Rho1 Arae
Ara IAU.svg
Cercle rouge 100%25.svg
The location of ρ1 Arae (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Ara
Right ascension 16h 56m 08.8405s [1]
Declination –50° 40′ 29.244″ [1]
Apparent magnitude  (V)6.275 [2]
Characteristics
Spectral type B3 Vnpe
U−B color index –0.691 [2]
B−V color index +0.008 [2]
Astrometry
Radial velocity (Rv)+19 [3]  km/s
Proper motion (μ)RA: –7.66 [1]   mas/yr
Dec.: –9.79 [1]   mas/yr
Parallax (π)5.06 ± 0.39  mas [1]
Distance 640 ± 50  ly
(200 ± 20  pc)
Absolute magnitude  (MV)−0.16 [4]
Details
Mass 6.3 ± 0.1 [5]   M☉
Luminosity 1,418 [6]   L☉
Surface gravity (log g)3.75 [7]   cgs
Temperature 19,800 [7]   K
Rotational velocity (v sin i)370 ± 10 [8]  km/s
Age 18.4 ± 1.5 [5]   Myr
Other designations
ρ1 Ara, V846 Arae, CD–50 10905, GC 22790, HD  152478, HIP 82868, HR 6274, NSV 8047, SAO 244280 [9]
Database references
SIMBAD data

Rho1 Arae is the Bayer designation for a star in the southern constellation of Ara. Unusually for a star with a Bayer designation, it was not catalogued by Bayer in his Uranometria . It was instead first catalogued by Nicolas Lacaille, in his Coelum Australe Stelliferum published in 1763. This star gained the Bayer designation of Rho1 Arae in Bode's Uranographia , published in 1801. Rho1 Arae is one of the dimmest stars with a Bayer designation, having an apparent visual magnitude of just +6.275 [2] According to the Bortle Dark-Sky Scale, this means the star is just barely visible to the naked eye in dark rural skies. Based upon parallax measurements, it is about 640 light-years (200 parsecs ) distant from the Sun, give or take a 50-light-year margin of error. [1]

A light curve for V846 Arae, plotted from TESS data V846AraLightCurve.png
A light curve for V846 Arae, plotted from TESS data

This is a spectroscopic binary system, which means that the presence of an orbiting companion is indicated by shifts in the spectrum. However, because the primary component is spinning rapidly with a projected rotational velocity of 370 ± 10, it is difficult to obtain reliable orbital elements. The orbital period has been estimated at 0.439 day. The spectrum of this system matches a stellar classification of B3 Vnpe, which may indicate the primary is a B-type main-sequence star. The 'e' suffix indicates the presence of emission lines, indicating this is a Be star. For Rho1 Arae, the emission lines are prominent and variable. [8]

Rho1 Arae has a peculiar velocity of 27.4 ± 4.9 km/s relative to its neighbors, [5] making it a runaway star system. A scenario that it was ejected from the Scorpius–Centaurus OB association as a result of a past supernova explosion seems unlikely because of its binarity. [8]

Related Research Articles

Rho Scorpii

Rho Scorpii is a double star in the constellation of Scorpius. It has an apparent visual magnitude of +3.87, which is bright enough to be seen with the naked eye. Based upon parallax measurements, it is located approximately 472 light years from the Sun. At that distance, the visual magnitude of the system is reduced by 0.07 due to extinction from interstellar dust. It is a member of the Upper Scorpius OB association.

Iota<sup>1</sup> Scorpii Star in the constellation Scorpius

Iota1 Scorpii, Latinized from ι1 Scorpii, is star in the southern constellation of Scorpius. With an apparent visual magnitude of 3.03, this star can be seen with the naked eye. It is sometimes called by the proper name Apollyon. Parallax measurements place it at a distance of roughly 1,930 light-years from Earth, with a 9% margin of error.

Rho Telescopii is the Bayer designation for an astrometric binary star system in the southern constellation of Telescopium. It is visible to the naked eye, with an apparent visual magnitude of +5.17. Based upon an annual parallax shift of 17.63 mas as measured from Earth, it is located approximately 185 light years from the Sun.

Epsilon Apodis Star in the constellation Apus

Epsilon Apodis, Latinized from ε Apodis, is the Bayer designation for a star in the southern circumpolar constellation of Apus. It has an apparent visual magnitude of 5.06, which is bright enough to be viewed from dark suburban skies. Based upon parallax measurements, it is at a distance of roughly 640 light-years from Earth.

Rho Aquarii Star in the constellation Aquarius

Rho Aquarii, Latinized from ρ Aquarii, is the Bayer designation for a binary star system in the equatorial constellation of Aquarius. It is visible to the naked eye with an apparent visual magnitude of +5.34. Based upon parallax measurements, this star is at a distance of roughly 870 light-years from Earth. It is drifting closer with a radial velocity of –9 km/s. The proximity of this star to the ecliptic means it is subject to lunar occultations.

Theta Arae Star in the constellation Ara

Theta Arae, Latinized from θ Arae, is the Bayer designation for a star in the constellation Ara. It has an apparent visual magnitude of +3.67, which is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 4.01 mas, Theta Arae is 810 light-years distant from the Earth.

Iota Arae Star in the constellation Ara

Iota Arae, Latinized from ι Arae, is the Bayer designation for a star in the southern constellation of Ara. It is approximately 930 light-years from Earth, give or take a 70 light-year margin of error, and has an apparent visual magnitude of 5.25. Based upon the Bortle Dark-Sky Scale, this means the star is visible to the naked eye from suburban skies.

V539 Arae Triple star system in the constellation Ara

V539 Arae (Bayer designation Nu1 Arae (ν1 Arae / ν1 Ara)) is a triple star system in the southern constellation of Ara. Based upon an annual parallax shift of 3.30 ± 0.47, this system is at a distance of roughly 1,000 light-years (310 parsecs) from Earth.

Sigma Centauri, Latinized from σ Centauri, is the Bayer designation for a solitary star in the southern constellation of Centaurus. It is visible to the naked eye with an apparent visual magnitude of 3.91. A visual companion at an angular separation of 88.11±0.37 mas along a position angle of 14.33°±2.59° was detected in 2010 using interferometry, but its association with Sigma Centauri remains undetermined as of 2013. The distance to Sigma Centauri, based upon an annual parallax shift of 7.92 mas, is around 412 light years.

Tau Librae, Latinized from τ Librae, is the Bayer designation for a binary star system at the southern edge of the zodiac constellation of Libra. It can be seen with the naked eye, having an apparent visual magnitude of 3.68. The distance to this system is around 367 light years, as determined from an annual parallax shift of 8.89 mas.

HD 153261 Star in the constellation Ara

HD 153261 is the Henry Draper Catalogue designation for a star in the southern constellation of Ara. It has an apparent visual magnitude of 6.137, placing it near the threshold of naked eye visibility. According to the Bortle Dark-Sky Scale, it can be viewed from dark suburban or rural skies. Based upon an annual parallax shift of just 2.32 mas, it is located at a distance of around 1,400 light-years from Earth.

Kappa<sup>1</sup> Apodis Star in the constellation Apus

Kappa1 Apodis, Latinized from κ1 Apodis, is the Bayer designation for a binary star system in the southern circumpolar constellation of Apus. Based upon parallax measurements, it is located roughly 1,200 light-years from Earth. The combined apparent visual magnitude of the system is 5.52, indicating that this is a faint, naked eye star that can be viewed in dark suburban skies. It is moving away from the Sun with a radial velocity of +62 km/s.

Beta Muscae Star in the constellation Musca

Beta Muscae, Latinized from β Muscae, is a binary star in the southern circumpolar constellation of Musca. With a combined apparent visual magnitude of 3.07, it is the second brightest star in the constellation. Judging by the parallax results, it is located at a distance of roughly 340 ± 13 light-years from the Earth.

2 Scorpii is a double star in the southern zodiac constellation of Scorpius. The brighter component has an apparent visual magnitude of 4.69, which is bright enough to be visible to the naked eye, while the fainter star is of magnitude 6.98. The distance to this pair can be estimated from the annual parallax shift of 6.49±0.51 mas, which places it roughly 500 light years away. It has a peculiar velocity of 16.5±2.4 km/s and is moving closer to the Sun with a heliocentric radial velocity of about −9 km/s, which will bring it to a perihelion distance of 450 ly (139 pc) in about 2.9 million years. This is a probable member of the Lower Centaurus–Crux group of the nearby Scorpius–Centaurus association, or else it is a member of the Gould's Belt.

HD 134687 is a binary star system in the southern constellation Lupus. It is visible to the naked eye with an apparent visual magnitude of 4.81. The distance to HD 134687 can be estimated from its annual parallax shift of 7.6 mas, yielding roughly 430 light years. It is a member of the ~11 million year old Upper Centaurus–Lupus subgroup of the Scorpius–Centaurus association, the closest OB association to the Sun.

4 Persei 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.

HD 70555 Star in the constellation Puppis

HD 70555 is a class K2.5II-III star in the constellation Puppis. Its apparent magnitude is 4.83 and it is approximately 1,010 light years away based on parallax.

N Scorpii is a star in the constellation Scorpius. Its apparent magnitude is 4.23, and was initially given the Bayer designation Alpha Normae by Lacaille but later moved from Norma to Scorpius. N Scorpii is located 550 light years away based on parallax, and is part of the Upper Scorpius–Centaurus association

V1073 Scorpii Variable star in the constellation Scorpius

V1073 Scorpii is a variable star in the constellation Scorpius. It has a non-Greek Bayer designation of k Scorpii. The star has a blue-white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around +4.87. Parallax measurements yield a distance estimate of approximately 2,920 ly (896 pc) from the Sun, and it is drifting further away with a radial velocity of +7 km/s. It has an absolute magnitude of −6.8

HD 83058 is a subgiant star in the constellation Vela and a spectroscopic binary. It is visible to the naked eye with an apparent visual magnitude of 5.0. Based upon an annual parallax shift of 3.4254 mas, it is located 950 light-years from the Sun. The system is moving further away with a heliocentric radial velocity of +35 km/s.

References

  1. 1 2 3 4 5 6 van Leeuwen, F. (November 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 Kozok, J. R. (September 1985), "Photometric observations of emission B-stars in the southern Milky Way", Astronomy and Astrophysics Supplement Series, 61: 387–405, Bibcode:1985A&AS...61..387K.
  3. ↑ Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick (eds.), Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, vol. 30, University of Toronto: International Astronomical Union, p. 57, Bibcode:1967IAUS...30...57E.
  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.
  5. 1 2 3 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 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.
  6. ↑ Hohle, M. M.; Neuhäuser, R.; Schutz, B. F. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349, arXiv: 1003.2335 , Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID   111387483.
  7. 1 2 Soubiran, C.; Le Campion, J.-F.; Cayrel de Strobel, G.; Caillo, A. (June 2010), "The PASTEL catalogue of stellar parameters", Astronomy and Astrophysics, 515: A111, arXiv: 1004.1069 , Bibcode:2010A&A...515A.111S, doi:10.1051/0004-6361/201014247, S2CID   118362423.
  8. 1 2 3 Jilinski, E.; et al. (September 2010), "A Dynamical Study of Suspected Runaway Stars as Traces of Past Supernova Explosions in the Region of the Scorpius–Centaurus OB Association", The Astrophysical Journal, 721 (1): 469–477, Bibcode:2010ApJ...721..469J, doi: 10.1088/0004-637X/721/1/469 .
  9. ↑ "rho01 Ara". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2012-08-01.{{cite web}}: CS1 maint: postscript (link)
  10. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
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