Astronomy:DI Chamaeleontis

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Short description: Star in the constellation Chamaleon
DI Chamaeleontis
280px
Image showing DI Cha A and B, each of which is also an even closer binary, and the surrounding nebulosity.
Observation data
{{#ifeq:J2000|J2000.0 (ICRS)|Epoch J2000.0      Equinox J2000.0 (ICRS)| Epoch J2000      [[Astronomy:Equinox (celestial coordinates)|Equinox J2000}}
Constellation Chamaeleon
A
Right ascension  11h 07m 20.72761s[1]
Declination −77° 38′ 07.3081″[1]
Apparent magnitude (V) 10.72[2]
A
Right ascension  11h 07m 20.18917s[3]
Declination −77° 38′ 11.5657″[3]
Apparent magnitude (V) 16.7[2]
Characteristics
Spectral type G0e[4] (G2 + M6 + M5.5 + M5.5)[5]
U−B color index +0.630[6]
B−V color index +1.144[6]
Variable type T Tau[7]
Astrometry
A
Radial velocity (Rv)+12.040±0.140[8] km/s
Proper motion (μ) RA: −22.552[1] mas/yr
Dec.: +1.214[1] mas/yr
Parallax (π)5.2913 ± 0.0133[1] mas
Distance616 ± 2 ly
(189.0 ± 0.5 pc)
B
Radial velocity (Rv)+15.5±0.3[9] km/s
Proper motion (μ) RA: −21.477 mas/yr
Dec.: +1.289 mas/yr
Parallax (π)5.2190 ± 0.0719[3] mas
Distance625 ± 9 ly
(192 ± 3 pc)
Details[10]
Aa
Mass1.7 M☉
Radius2.00 R☉
Luminosity4.7 L☉
Temperature6,030 K
Age7.1 Myr
Ba/Bb
Mass0.18 M☉
Radius1.13 R☉
Luminosity0.11 L☉
Temperature3,130 K
Age3.0 Myr
Other designations
DI Cha, HIP 54365, CD−76°486, WDS J11073-7738, AAVSO 1104-77
Database references
SIMBADdata
B

DI Chamaeleontis, also known as Hen 3-593 or HIP 54365, is a quadruple star system in the constellation Chamaeleon. The system is located 616 light years away from Earth based on Gaia DR3 parallax measurements.[1]

A light curve for DI Chamaeleontis, plotted from TESS data,[11]

DI Cha is a variable star of the T Tauri type, young stellar objects just approaching the main sequence. It varies erratically between visual magnitudes 10.65 and 10.74.[7] Although it is visually faint, it was noticed because of the prominent emission lines in its spectrum.[12]

In 1977, DI Cha was observed to have a much fainter companion.[13] The separation was later measured at 4.6", approximately 644 astronomical units (AU).[14] The B component was discovered to be a pair of stars separated by only 0.066", about 10 AU,[15] both with spectral type M5.5.[5] Finally, the variable primary star was found to have a faint companion 0.2" (therefore ~30 AU) away, of spectral type M6.[5]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 Tokovinin, Andrei (2018). "The Updated Multiple Star Catalog". The Astrophysical Journal Supplement Series 235 (1): 6. doi:10.3847/1538-4365/aaa1a5. Bibcode: 2018ApJS..235....6T. 
  3. ↑ 3.0 3.1 3.2 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  4. ↑ Torres, C. A. O.; Quast, G. R.; Da Silva, L.; de la Reza, R.; Melo, C. H. F.; Sterzik, M. (2006). "Search for associations containing young stars (SACY). I. Sample and searching method". Astronomy and Astrophysics 460 (3): 695. doi:10.1051/0004-6361:20065602. Bibcode: 2006A&A...460..695T. 
  5. ↑ 5.0 5.1 5.2 Schmidt, T. O. B.; Vogt, N.; Neuhäuser, R.; Bedalov, A.; Roell, T. (2013). "New companions in the stellar systems of DI Cha, Sz 22, CHXR 32, and Cha Hα 5 in the Chamaeleon I star-forming region". Astronomy & Astrophysics 557: A80. doi:10.1051/0004-6361/201220660. Bibcode: 2013A&A...557A..80S. 
  6. ↑ 6.0 6.1 Kilkenny, D.; Whittet, D. C. B.; Davies, J. K.; Evans, A.; Bode, M. F.; Robson, E. I.; Banfield, R. M. (1985). "Optical and infrared photometry of southern early-type shell stars and pre-main-sequence variables". In Its South African Astronomical Observatory Circular No. 9 P 55-86 (SEE N86-18271 08-89) 9: 55. Bibcode: 1985SAAOC...9...55K. 
  7. ↑ 7.0 7.1 Samus, N. N. 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. Bibcode: 2009yCat....102025S. 
  8. ↑ Nguyen, Duy Cuong; Brandeker, Alexis; van Kerkwijk, Marten H.; Jayawardhana, Ray (February 2012). "Close Companions to Young Stars. I. A Large Spectroscopic Survey in Chamaeleon I and Taurus-Auriga". The Astrophysical Journal 745 (2): 25. doi:10.1088/0004-637X/745/2/119. 119. Bibcode: 2012ApJ...745..119N. 
  9. ↑ Gutiérrez Albarrán, M. L. et al. (2020). "The Gaia-ESO Survey: Calibrating the lithium-age relation with open clusters and associations. I. Cluster age range and initial membership selections". Astronomy and Astrophysics 643: A71. doi:10.1051/0004-6361/202037620. Bibcode: 2020A&A...643A..71G. 
  10. ↑ Daemgen, S.; Petr-Gotzens, M. G.; Correia, S.; Teixeira, P. S.; Brandner, W.; Kley, W.; Zinnecker, H. (2013). "Protoplanetary disk evolution and stellar parameters of T Tauri binaries in Chamaeleon I". Astronomy & Astrophysics 554: A43. doi:10.1051/0004-6361/201321220. Bibcode: 2013A&A...554A..43D. 
  11. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  12. ↑ Henize, Karl G. (1963). "Emission-Line Stars in an Obscured Region in Chamaeleon". Astronomical Journal 68: 280. doi:10.1086/109141. Bibcode: 1963AJ.....68S.280H. http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1963AJ.....68S.280H&link_type=ARTICLE&db_key=AST&high=. 
  13. ↑ Schwartz, R. D. (1977). "A survey of southern dark clouds for Herbig-Haro objects and H-alpha emission stars". Astrophysical Journal Supplement Series 35: 161. doi:10.1086/190473. Bibcode: 1977ApJS...35..161S. 
  14. ↑ Reipurth, Bo; Zinnecker, Hans (1993). "Visual binaries among pre-main sequence stars". Astronomy and Astrophysics 278: 81. Bibcode: 1993A&A...278...81R. 
  15. ↑ Lafrenière, David; Jayawardhana, Ray; Brandeker, Alexis; Ahmic, Mirza; Van Kerkwijk, Marten H. (2008). "A Multiplicity Census of Young Stars in Chamaeleon I". The Astrophysical Journal 683 (2): 844–861. doi:10.1086/590239. Bibcode: 2008ApJ...683..844L. 



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