To install click the Add extension button. That's it.

The source code for the WIKI 2 extension is being checked by specialists of the Mozilla Foundation, Google, and Apple. You could also do it yourself at any point in time.

4,5
Kelly Slayton
Congratulations on this excellent venture… what a great idea!
Alexander Grigorievskiy
I use WIKI 2 every day and almost forgot how the original Wikipedia looks like.
Live Statistics
English Articles
Improved in 24 Hours
Added in 24 Hours
Languages
Recent
Show all languages
What we do. Every page goes through several hundred of perfecting techniques; in live mode. Quite the same Wikipedia. Just better.
.
Leo
Newton
Brights
Milds

From Wikipedia, the free encyclopedia

R Arae

A visual band light curve for R Arae, adapted from Blane et al. (2019)[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Ara
Right ascension 16h 39m 44.726s[2]
Declination −56° 59′ 39.92″[2]
Apparent magnitude (V) 6.17 (- 6.20) - 7.32[3]
Characteristics
Spectral type B9Vp[4] (B5V + F1IV[5])
B−V color index 0.10[5]
Variable type Algol[4]
Astrometry
Radial velocity (Rv)+5.5[5] km/s
Proper motion (μ) RA: −4.991[6] mas/yr
Dec.: −17.810[6] mas/yr
Parallax (π)3.3603 ± 0.0647 mas[6]
Distance970 ± 20 ly
(298 ± 6 pc)
Absolute magnitude (MV)−0.48 + 0.00[5]
Orbit[5]
Period (P)4.425 d
Eccentricity (e)0
Inclination (i)78.0°
Semi-amplitude (K1)
(primary)
55.3 km/s
Semi-amplitude (K2)
(secondary)
181.6 km/s
Details[5]
A
Mass5.0 M
Radius3.41 R
Luminosity257 L
Surface gravity (log g)4.07 cgs
Temperature12,500 K
Rotational velocity (v sin i)202[5] km/s
B
Mass1.5 M
Radius5.97 R
Luminosity78 L
Surface gravity (log g)3.07 cgs
Temperature7,000 K
Rotational velocity (v sin i)73 km/s
Other designations
HIP 81589, CD-56°6482, SAO 244037, HD 149730
Database references
SIMBADdata

R Arae is an Algol-type eclipsing binary in the constellation Ara. Located approximately 298 parsecs (970 ly) distant, it normally shines at magnitude 6.17, but during eclipses can fall as low as magnitude 7.32.[3] It has been suggested by multiple studies that mass transfer is occurring between the two stars of this system,[7][8] and the period of eclipses seems to be increasing over time.[8] The primary is a blue-white main sequence star of spectral type B5V that is 5 times as massive as the Sun, while the secondary is a yellow-white star of spectral type F1IV that is 1.5 times as massive as the Sun. Stellar material is being stripped off the secondary and accreting on the primary.[5]

R Arae has an 8th-magnitude companion 3 away.[5] The companion star is at a similar distance.[9]

YouTube Encyclopedic

  • 1/2
    Views:
    13 405
    15 830
  • Section, Week 3
  • Section, Week 2

Transcription

References

  1. ^ Blane, D.; Blackford, M. G.; Budding, E.; Reed, P. A. (May 2019). "New light on R Arae" (PDF). Information Bulletin on Variable Stars. 6267 (1). doi:10.22444/IBVS.6267. S2CID 202939949. Retrieved 24 October 2021.
  2. ^ a b 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.
  3. ^ a b VSX (25 October 2010). "R Arae". AAVSO Website. American Association of Variable Star Observers. Retrieved 30 June 2014.
  4. ^ a b Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
  5. ^ a b c d e f g h i Bakıș, H.; Bakıș, V.; Eker, Z.; Demircan, O. (2016). "Active binary R Arae revisited: Bringing the secondary component to light and physical modelling of the circumstellar material". Monthly Notices of the Royal Astronomical Society. 458 (1): 508–516. Bibcode:2016MNRAS.458..508B. doi:10.1093/mnras/stw320.
  6. ^ a b c 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.
  7. ^ Nield, K. M. (1991). "Observations and analysis of the Southern binary R Arae". Astrophysics and Space Science. 180 (2): 233–252. Bibcode:1991Ap&SS.180..233N. doi:10.1007/BF00648180. S2CID 122896654.
  8. ^ a b Reed, P. A.; McCluskey Jr., G. E.; Kondo, Y.; Sahade, J.; Guinan, E. F.; GiméNez, A.; Caton, D. B.; Reichart, D. E.; Ivarsen, K. M.; Nysewander, M. C. (2010). "Ultraviolet study of the active interacting binary star R Arae using archivalIUEdata". Monthly Notices of the Royal Astronomical Society. 401 (2): 913. arXiv:0909.4047. Bibcode:2010MNRAS.401..913R. doi:10.1111/j.1365-2966.2009.15741.x. S2CID 15237238.
  9. ^ 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.
This page was last edited on 15 July 2023, at 17:52
Basis of this page is in Wikipedia. Text is available under the CC BY-SA 3.0 Unported License. Non-text media are available under their specified licenses. Wikipedia® is a registered trademark of the Wikimedia Foundation, Inc. WIKI 2 is an independent company and has no affiliation with Wikimedia Foundation.