emamajek on 01-May-2020 20:20:32 GMT about HD 110810
HD 110810 is part of a multiple system WDS J12452-5721, although only components A and C appear to constitute a physical binary
WDS J12452-5721A = Gaia DR2 6060965699625586176 = HD 110810
WDS J12452-5721B = Gaia DR2 6092573252981419776 = HD 124364 = HIP 69570
WDS J12452-5721C = Gaia DR2 6060965630906108672 = 2MASS J12451698-5721348
multiplicity and double star designations are currently missing from SIMBAD
However, the physical connection between B and A+C seems unlikely. Shaya & Olling 2011 (2011ApJS..192....2S) pair A and B (HIP 62229 and HIP 69570), and note that they are separated by 20 pc. Here is a comparison of their Gaia DR2 photometry:
pmRA(A)=-201.033+-0.052, pmDec(A)=-131.548+-0.046, plx(A)=50.4844+-0.0450mas
pmRA(B)=-102.218+-0.095, pmDec(B)=-121.897+-0.120, plx(B)=26.4256+-0.0610mas
pmRA(C)=-200.177+-0.105, pmDec(C)=-140.604+-0.097, plx(C)=50.3287+-0.0895mas
Note that A (HD 110810) is clearly active (logR'HK=-4.42; Jenkins+2006) and slightly metal enhanced ([Fe/H]=-0.11; Hinkel+2017), but B (HD 124364) is relatively inactive (logR'HK=-4.828; Gomes da Silva+2014), metal poor ([Fe/H]=-0.27+-0.01; Sousa+2008), and slow rotating (vsini = 1.0 km/s; Meunier+2017). Astrophysically B appears to be much older than A, and they are unlikely to be conatal.
Tian+2020 (2020ApJS..246....4T) consider A and C to share common proper motion based on Gaia DR2 astrometry: physical separation 433.337 au, projected separation 21.80926".
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