Abstract:
We present the study of four far-ultraviolet (FUV) bright stars in the field of the open cluster NGC 2420 using the
Ultra Violet Imaging Telescope mounted on AstroSat. The three stars 525, 527, and 560 are members, while star
646 is a nonmember of the cluster. To characterize and determine the parameters of these stars, multiwavelength
spectral energy distributions (SEDs) are analyzed using UV, optical, and IR data sets. For all four FUV bright stars,
a two-component SED model fits well. Our findings indicate that two stars, 525 and 560, are binary blue straggler
star (BSS) systems. These BSS systems may have formed in a tertiary system due to mass transfer from an evolved
outer tertiary companion. Star 527 is a binary system of a BSS and an extremely low-mass (ELM) white dwarf,
while star 646 is a binary system of a horizontal branch star and an ELM white dwarf. The effective temperatures,
radii, luminosities, and masses of the two ELMs are (10250, 11500) K (0.42, 0.12) Re, (1.61, 0.23) Le, and (0.186,
0.170) Me, respectively. The star 527 could be a post-mass-transfer system and may have originated through the
Case A/B mass-transfer process in a low-density environment. The cooling age of the ELMs is < 1 Myr,
indicating that they have only recently formed.
