HD 135530 hasevolved into ared giant on theasymptotic giant branch, meaning that it has exhausted its core helium and is fusing hydrogen and helium in shells outside the core.[5] Its photosphere has expanded to 79 R☉ at aneffective temperature of3820K and shows a spectrum classified as M2IIIa, withIIIa indicating a star slightly more luminous than a typical giant.
Although listed only as a suspected variable in theGeneral Catalogue of Variable Stars, observations by theMASCARA team have shown that its brightness is in fact variable, with a period of about 20 days.[1]
^Hoffleit, D.; Warren Jr, W. H. (1991).Bright Star Catalogue (5th Revised (Preliminary Version) ed.). Astronomical Data Center, NSSDC/ADC. Retrieved2015-08-17.
^Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)".Catalogue of Eggen's UBV Data. SIMBAD.Bibcode:1986EgUBV........0M.
^ab"NSV 20281".The International Variable Star Index. AAVSO. Retrieved21 April 2025.
^abcAnders, 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.S2CID131780028.
