Mira variables are often masquerading as novae in the nearby galaxies. In this paper we discuss t... more Mira variables are often masquerading as novae in the nearby galaxies. In this paper we discuss this problem and focus on two Mira variables in M31 galaxy, one of them classified as nova by our team during novae search in M31 galaxy. Astrometry and photometry data, finding charts and light curves are presented.
Massive stellar content of stellar complexes and associations in M 33 is studied combining deep U... more Massive stellar content of stellar complexes and associations in M 33 is studied combining deep UBV photometry from the Local Group Survey (Massey et al. 2006) and JHK photometry from the 2MASS. Two basic populations (incl. OB stars and red supergiants) are distinguished and their application for reconstruction of the star formation process in this galaxy are discussed.
Mira variables are often masquerading as novae in the nearby galaxies. In this paper we discuss t... more Mira variables are often masquerading as novae in the nearby galaxies. In this paper we discuss this problem and focus on two Mira variables in M31 galaxy, one of them classified as nova by our team during novae search in M31 galaxy. Astrometry and photometry data, finding charts and light curves are presented.
Massive stellar content of stellar complexes and associations in M 33 is studied combining deep U... more Massive stellar content of stellar complexes and associations in M 33 is studied combining deep UBV photometry from the Local Group Survey (Massey et al. 2006) and JHK photometry from the 2MASS. Two basic populations (incl. OB stars and red supergiants) are distinguished and their application for reconstruction of the star formation process in this galaxy are discussed.
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Papers by Nina Taneva