R Fornacis

R Fornacis is a topic that has captured the attention of millions of people around the world. Since its emergence, it has generated debates, controversies and has been the subject of numerous studies and research. Its impact on society has been profound, and its relevance remains as current as in its beginnings. In this article, we will explore in detail the different facets of R Fornacis, from its origins to its current situation, as well as its possible implications for the future. Through a deep and objective analysis, we will try to shed light on this topic that has influenced so much in different aspects of modern life.

R Fornacis

The visual band light curve of R Fornacis, from AAVSO data[1]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Fornax
Right ascension 02h 29m 15.308s[2]
Declination −26° 05′ 55.65″[2]
Apparent magnitude (V) 7.5 - 13.0[3]
Characteristics
Evolutionary stage AGB[4]
Spectral type C4,3e[5]
Apparent magnitude (J) 3.82[6]
Apparent magnitude (K) 1.06[6]
Variable type Mira[3]
Astrometry
Proper motion (μ) RA: 8.551[2] mas/yr
Dec.: −3.957[2] mas/yr
Parallax (π)1.8069±0.0358 mas[2]
Distance1,810 ± 40 ly
(550 ± 10 pc)
Details
Mass1.05[7] M☉
Radius575[8][a] R☉
Luminosity5,800[8] L☉
Surface gravity (log g)0.12[7] cgs
Temperature2,100[8] K
Metallicity 0.21[7] dex
Other designations
R For, CD−26°892, IRAS 02270-2619, 2MASS J02291531-2605559
Database references
SIMBADdata

R Fornacis is a Mira variable and carbon star located in the constellation Fornax. It is around 1,800 light years away based on parallax measurements.

R Fornacis is a carbon star, a star on the asymptotic giant branch with an excess of carbon over oxygen in its atmosphere due to fusion products being dredged up to the surface from deep inside the star. It is also a Mira variable, a type of pulsating giant star which varies by several apparent magnitudes with a period of a few hundred days. R Fornacis has a period of 389 days and varies between extremes of magnitude 7.5 and 13.0, although average maximum and minimum magnitudes are 8.9 and 12.2 respectively.[9]

R Fornacis was discovered to be variable in 1896 after it had been observed with a different brightness to that shown in the Cordoba Durchmusterung.[10] In 1983, an unusually deep minimum was observed, and later correlated with an asymmetric shell of material ejected from the surface of the star.[4] Unconfirmed visual estimates of the unusual minimum give a magnitude of 14.0, while infrared observations confirm the unusual variation.[9]

Possible planetary system

A study led by C. Paladini, using near-infrared interferometry at the Very Large Telescope, detected a photocenter shift between R Fornacis and an object on its circumstellar envelope. This might be caused by a dust blob that moves around the circumstellar dust, or by a Jovian-mass companion (~1 MJ), with an orbital period around R Fornacis of 185 years.[4]

Notes

  1. ^ Applying the Stefan–Boltzmann law with a nominal solar effective temperature of 5,772 K:
    .

References

  1. ^ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
  2. ^ a b c d e 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. ^ 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.
  4. ^ a b c Paladini, C.; Sacuto, S.; Klotz, D.; Ohnaka, K.; Wittkowski, M.; Nowotny, W.; Jorissen, A.; Hron, J. (2012). "Detection of an asymmetry in the envelope of the carbon Mira R Fornacis using VLTI/MIDI". Astronomy & Astrophysics. 544: L5. arXiv:1207.3910. Bibcode:2012A&A...544L...5P. doi:10.1051/0004-6361/201219831. S2CID 54598068.
  5. ^ Yamashita, Y. (1975). "The C-classification of spectra of carbon stars. II". Tokyo. 15: 47. Bibcode:1975AnTok..15...47Y.
  6. ^ a b Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  7. ^ a b c Anders, F.; Khalatyan, A.; Chiappini, C.; Queiroz, A. B.; Santiago, B. X.; Jordi, C.; Girardi, L.; Brown, A. G. A.; Matijevič, G.; Monari, G.; Cantat-Gaudin, T.; Weiler, M.; Khan, S.; Miglio, A.; Carrillo, I.; Romero-Gómez, M.; Minchev, I.; De Jong, R. S.; Antoja, T.; Ramos, P.; Steinmetz, M.; Enke, H. (2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy and Astrophysics. 628: A94. arXiv:1904.11302. Bibcode:2019A&A...628A..94A. doi:10.1051/0004-6361/201935765. S2CID 131780028.
  8. ^ a b c Siderud, Emelie (2020). Dust emission modelling of AGB stars.
  9. ^ a b Feast, M. W.; Whitelock, P. A.; Catchpole, R. M.; Roberts, G.; Overbeek, M. D. (1984). "Variable circumstellar obscuration of the carbon star R Fornacis". Monthly Notices of the Royal Astronomical Society. 211 (2): 331–337. doi:10.1093/mnras/211.2.331.
  10. ^ Pickering, E. C.; Leland, E. F. (1896). "Harvard College Observatory, circular no. 10. Six new variable stars". The Astrophysical Journal. 4: 234. Bibcode:1896ApJ.....4..234P. doi:10.1086/140271.