RS Telescopii

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RS Telescopii
RSTelLightCurve.png
A visual band light curve for RS Telescopii, plotted from AAVSO data [1]
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Telescopium
Right ascension 18h 18m 51.2224s [2]
Declination −46° 32′ 53.427″ [2]
Apparent magnitude  (V)10.67 [3]
Characteristics
Spectral type R0
B−V color index 2.100±0.510 [3]
Variable type R CrB [4]
Astrometry
Radial velocity (Rv)−3.0 [3]  km/s
Proper motion (μ)RA: −2.730 [2]   mas/yr
Dec.: −6.670 [2]   mas/yr
Parallax (π)0.1732 ± 0.0166  mas [2]
Distance 19,000 ± 2,000  ly
(5,800 ± 600  pc)
Details
Radius 73 [5]   R☉
Luminosity 288 (at max) [6]   L☉
Surface gravity (log g)1.0 [7]   cgs
Temperature 5,800 [6]   K
Other designations
RS Tel, CD−46°12279, HIP  89739 [8]
Database references
SIMBAD data

RS Telescopii, abbreviated RS Tel, is a variable star in the southern constellation of Telescopium. It is a dim star with an apparent visual magnitude of 10.67, [3] which is much too faint to be visible without a telescope. The variability of this star was discovered by Evelyn F. Leland and announced by Edward C. Pickering in 1910. [9] It was first studied by Cecilia H. Payne in 1928 at the Harvard College Observatory. [10] [11]

This is an R-type carbon star with a class of R0. [12] RS Tel is a typical R Coronae Borealis variable [10] —an extremely hydrogen-deficient supergiant thought to have arisen as the result of the merger of two white dwarfs; fewer than 100 have been discovered as of 2012. [4] It has under 55% [13] the mass of the Sun and an effective temperature of around 5,800 K. [6] The spectrum of the star shows anomalously weak lines of hydrogen, with strong lines of C2, CN, and neutral carbon. [14]

RS Tel has a maximum magnitude of 9.6 and a minimum magnitude 16.5. [15] The star undergoes large, random variations in brightness on a time scale of thousands of days with no apparent periodicity. [16] The star is surrounded by a circumstellar shell of dust which radiating an infrared excess. [16]

Related Research Articles

<span class="mw-page-title-main">Telescopium</span> Constellation in the southern celestial hemisphere

Telescopium is a minor constellation in the southern celestial hemisphere, one of twelve named in the 18th century by French astronomer Nicolas-Louis de Lacaille and one of several depicting scientific instruments. Its name is a Latinized form of the Greek word for telescope. Telescopium was later much reduced in size by Francis Baily and Benjamin Gould.

<span class="mw-page-title-main">R Coronae Borealis</span> Variable star in the constellation Corona Borealis

R Coronae Borealis is a low-mass yellow supergiant star in the constellation of Corona Borealis. It is the prototype of the R Cor Bor class of variable stars, which fade by several magnitudes at irregular intervals. R Coronae Borealis itself normally shines at approximately magnitude 6, just about visible to the naked eye, but at intervals of several months to many years fades to as faint as 15th magnitude. Over successive months it then gradually returns to its normal brightness, giving it the nickname "reverse nova", after the more common type of star which rapidly increases in brightness before fading.

<span class="mw-page-title-main">T Coronae Borealis</span> Recurrent nova in the constellation Corona Borealis

T Coronae Borealis, is a recurring nova in the constellation Corona Borealis. It was first discovered in outburst in 1866 by John Birmingham, although it had been observed earlier as a 10th magnitude star.

<span class="mw-page-title-main">DY Persei</span> Variable carbon star in the constellation Perseus

DY Persei is a variable star and carbon star in the Perseus constellation. At maximum it is 11th magnitude and at its faintest it drops to 16th magnitude. DY Persei is the prototype of the very rare DY Persei class of variables that pulsate like red variables but also fade from sight like R Coronae Borealis variables.

<span class="mw-page-title-main">S Coronae Borealis</span> Star in the constellation Corona Borealis

S Coronae Borealis is a Mira variable star in the constellation Corona Borealis. Its apparent magnitude varies between 5.3 and 13.6, with a period of 360 days—just under a year. Within the constellation, it lies to the west of Theta Coronae Borealis, and around 1 degree southeast of the eclipsing binary star U Coronae Borealis.

<span class="mw-page-title-main">U Aquarii</span> Star in the constellation of Aquarius

U Aquarii, abbreviated U Aqr, is a variable star in the equatorial constellation of Aquarius. It is invisible to the naked eye, having an apparent visual magnitude that ranges from 10.6 down to as low as 15.9. Based on parallax measurements, the distance to this star is approximately 38 kly (12 kpc). In 1990, W. A. Lawson and associates provided a distance estimate of 43 kly (13.2 kpc) based on the assumption of a bolometric magnitude of −5. It appears to lie several kiloparsecs below the galactic plane, and thus may belong to an old stellar population.

<span class="mw-page-title-main">UX Antliae</span> Star in the constellation Antlia


UX Antliae is a post-AGB and R Coronae Borealis variable star that has a base apparent magnitude of around 11.85, with irregular dimmings down to below magnitude 18.0.

<span class="mw-page-title-main">Delta Coronae Borealis</span> Yellow giant star in the constellation Corona Borealis

Delta Coronae Borealis, Latinized from δ Coronae Borealis, is a variable star in the constellation Corona Borealis. Its apparent magnitude varies regularly between apparent magnitude 4.57 and 4.69, and it is around 170 light-years distant.

<span class="mw-page-title-main">RY Sagittarii</span> Yellow supergiant star in the constellation Sagittarius

RY Sagittarii is a yellow supergiant and an R Coronae Borealis type variable star in the constellation Sagittarius. Although it ostensibly has the spectrum of a G-type star, it differs markedly from most in that it has almost no hydrogen and much carbon.

<span class="mw-page-title-main">Z Ursae Minoris</span> Star in the constellation Ursa Minor

Z Ursae Minoris is a carbon star and R Coronae Borealis variable in the constellation Ursa Minor.

<span class="mw-page-title-main">RX Telescopii</span> Red supergiant star in the constellation Telescopium

RX Telescopii is an irregular variable star in the constellation Telescopium. It has a maximum magnitude of 6.45 and a minimum magnitude 7.47. It is a red supergiant with a spectral type of M3Iab, indicating the star is an intermediate-size luminous supergiant star.

<span class="mw-page-title-main">PZ Telescopii</span> Star in the constellation Telescopium

PZ Telescopii, also known as HD 174429 or simply PZ Tel, is a young star in the constellation Telescopium. Based on parallax measurements, it is located at a distance of 154 light years from the Sun. The star is drifting closer with a radial velocity of −4 km/s. It is too faint to be visible to the naked eye and is classified as a BY Draconis variable that ranges in apparent visual magnitude from 8.33 down to 8.63 over a period of 22.581 hours. It is one of the closest and hence brightest pre-main-sequence stars to Earth.

<span class="mw-page-title-main">V Coronae Australis</span> Variable star in the constellation Corona Australis

V Coronae Australis is a R Coronae Borealis variable (RCB) star in the constellation Corona Australis. These are extremely hydrogen-deficient supergiants thought to have arisen as the result of the merger of two white dwarfs; fewer than 100 have been discovered as of 2012. V Coronae Australis dimmed in brightness from 1994 to 1998.

<span class="mw-page-title-main">WX Coronae Australis</span> Variable star in the constellation Corona Australis

WX Coronae Australis is an R Coronae Borealis star in the constellation Corona Australis, one of the brightest examples of this extremely rare class of variable star. Despite the rarity, Corona Australis hosts another R CrB star, V Coronae Australis.

<span class="mw-page-title-main">BL Telescopii</span> Star in the constellation Telescopium

BL Telescopii is a multiple star in the constellation Telescopium. An Algol-like eclipsing binary, the star system varies between apparent magnitudes 7.09 and 9.08 in just over 778 days, which is generally too faint to be seen with the unaided eye. This is mainly due to the system being an eclipsing binary. The eclipse itself dims the star by two magnitudes and lasts around 104 days.

<span class="mw-page-title-main">V Coronae Borealis</span> Mira-type long period variable star in the constellation Corona Borealis

V Coronae Borealis is a Mira-type long period variable star and carbon star in the constellation Corona Borealis. Its apparent magnitude varies between 6.9 and 12.6 over a period of 357 days

<span class="mw-page-title-main">Sigma Coronae Borealis</span> Star in the constellation Corona Borealis

Sigma Coronae Borealis is a star system in the constellation of Corona Borealis. It is a quintuple star system containing three sunlike main-sequence stars and two other low-mass stars. The combined visual magnitude is 5.3 and the system lies 74 light years from Earth. σ CrB A is the variable star TZ Coronae Borealis.

<span class="mw-page-title-main">W Coronae Borealis</span> Star in the constellation Corona Borealis

W Coronae Borealis is a Mira-type long period variable star in the constellation Corona Borealis. Its apparent magnitude varies between 7.8 and 14.3 over a period of 238 days.

Upsilon Coronae Borealis, Latinized from υ Coronae Borealis, is a solitary star in the northern constellation of Corona Borealis. It is a white-hued star that is dimly visible to the naked eye with an apparent visual magnitude of 5.78. The distance to this object is approximately 630 light-years based on parallax.

<span class="mw-page-title-main">S Apodis</span> Variable star in the constellation Apus

S Apodis, also known as HD 133444 is a variable star located in the southern circumpolar constellation Apus. It has an apparent magnitude ranging from 9.6 to 17, which is below the limit for naked eye visibility. The object is located relatively far at a distance of approximately 15,000 light years based on Gaia DR3 parallax measurements, but it is drifting closer with a heliocentric radial velocity of −75 km/s.

References

  1. ↑ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
  2. 1 2 3 4 5 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.
  3. 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.
  4. 1 2 Tisserand, P.; et al. (2012). "The Ongoing Pursuit of R Coronae Borealis Stars: ASAS-3 Survey Strikes Again". Astronomy & Astrophysics. 551: 22. arXiv: 1211.2475 . Bibcode:2013A&A...551A..77T. doi:10.1051/0004-6361/201220713. S2CID   59060842. A77.
  5. ↑ Stassun, Keivan G.; et al. (2019-10-01). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv: 1905.10694 . Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467. hdl: 1721.1/124721 . ISSN   0004-6256. S2CID   166227927.
  6. 1 2 3 Bergeat, J.; Knapik, A.; Rutily, B. (2002). "Carbon-rich giants in the HR diagram and their luminosity function". Astronomy and Astrophysics. 390 (3): 967. Bibcode:2002A&A...390..967B. doi: 10.1051/0004-6361:20020525 .
  7. ↑ Hema, B. P.; Pandey, Gajendra; Lambert, David L. (2012). "The Galactic R Coronae Borealis Stars: The C2 Swan Bands, the Carbon Problem, and the 12C/13C Ratio". The Astrophysical Journal. 747 (2): 102. arXiv: 1201.1357 . Bibcode:2012ApJ...747..102H. doi:10.1088/0004-637X/747/2/102. S2CID   118653032.
  8. ↑ "RS Tel". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-12-11.
  9. ↑ Pickering, Edward C. (March 1910). "20 new variable stars in Harvard Map, Nos. 2, 5, 32, 44 and 53". Astronomische Nachrichten. 184: 5. Bibcode:1910AN....184....5P. doi:10.1002/asna.19101840104.
  10. 1 2 Milone, Luis A. (October 1990). "Identification charts for southern R Coronae Borealis-stars". Astrophysics and Space Science. 172 (2): 263–271. Bibcode:1990Ap&SS.172..263M. doi:10.1007/BF00643318. S2CID   118353230.
  11. ↑ Payne, Cecilia H. (October 1928). "The R Coronae Type Variables RS Telescopii and Y Muscae". Harvard College Observatory Bulletin. 861: 11–12. Bibcode:1928BHarO.861...11P.
  12. ↑ Knapp, G.; et al. (May 2001). "Reprocessing the Hipparcos data for evolved giant stars II. Absolute magnitudes for the R-type carbon stars". Astronomy and Astrophysics. 371: 222–232. arXiv: astro-ph/0103141 . Bibcode:2001A&A...371..222K. doi:10.1051/0004-6361:20010348. S2CID   18248545.
  13. ↑ Stasińska, G.; Szczerba, R.; Schmidt, M.; Siódmiak, N. (2006). "Post-AGB stars as testbeds of nucleosynthesis in AGB stars". Astronomy and Astrophysics. 450 (2): 701. arXiv: astro-ph/0601504 . Bibcode:2006A&A...450..701S. doi:10.1051/0004-6361:20053553. S2CID   12040452.
  14. ↑ Bidelman, William P. (January 1953). "The Spectra of Certain Stars whose Atmospheres may be Deficient in Hydrogen". Astrophysical Journal. 117: 25. Bibcode:1953ApJ...117...25B. doi:10.1086/145665.
  15. ↑ BSJ (11 November 2011). "RX Telescopii". AAVSO Website. American Association of Variable Star Observers . Retrieved 26 June 2014.
  16. 1 2 Feast, M. W.; et al. (February 1997). "The R Coronae Borealis stars - I. Infrared photometry and long-term variations". Monthly Notices of the Royal Astronomical Society. 285 (2): 317–338. Bibcode:1997MNRAS.285..317F. doi: 10.1093/mnras/285.2.317 .
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