UOCS. XIII. Study of the Far-ultraviolet Bright Stars in the Open Cluster NGC 2420 Using AstroSat
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 param...
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad13e8 |
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| author | R. K. S. Yadav Arvind K. Dattatrey Geeta Rangwal Annapurni Subramaniam D. Bisht Ram Sagar |
| author_facet | R. K. S. Yadav Arvind K. Dattatrey Geeta Rangwal Annapurni Subramaniam D. Bisht Ram Sagar |
| author_sort | R. K. S. Yadav |
| collection | DOAJ |
| description | 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) R _⊙ , (1.61, 0.23) L _⊙ , and (0.186, 0.170) M _⊙ , 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. |
| first_indexed | 2024-03-08T09:23:18Z |
| format | Article |
| id | doaj.art-bd735cc6863d4a57901fcde58aa31c09 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-08T09:23:18Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-bd735cc6863d4a57901fcde58aa31c092024-01-31T11:33:15ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01961225110.3847/1538-4357/ad13e8UOCS. XIII. Study of the Far-ultraviolet Bright Stars in the Open Cluster NGC 2420 Using AstroSatR. K. S. Yadav0https://orcid.org/0000-0003-1342-9626Arvind K. Dattatrey1https://orcid.org/0000-0002-4729-9316Geeta Rangwal2https://orcid.org/0000-0002-6373-770XAnnapurni Subramaniam3https://orcid.org/0000-0003-4612-620XD. Bisht4https://orcid.org/0000-0002-8988-8434Ram Sagar5https://orcid.org/0000-0003-4973-4745Aryabhatta Research Institute of Observational Sciences , Manora Peak, Nainital 263002, India ; arvind@aries.res.in, rkant@aries.res.inAryabhatta Research Institute of Observational Sciences , Manora Peak, Nainital 263002, India ; arvind@aries.res.in, rkant@aries.res.in; Deen Dayal Upadhyay Gorakhpur University , Gorakhpur, Uttar Pradesh 273009, IndiaSouth-Western Institute for Astronomy Research, Yunnan University , Kunming 650500, People's Republic of ChinaIndian Institute of Astrophysics , Koramangala, Bangalore 560034, IndiaIndian Centre for Space Physics , 466 Barakhola, Singabari road, Netai Nagar, Kolkata 700099, IndiaIndian Institute of Astrophysics , Koramangala, Bangalore 560034, IndiaWe 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) R _⊙ , (1.61, 0.23) L _⊙ , and (0.186, 0.170) M _⊙ , 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.https://doi.org/10.3847/1538-4357/ad13e8Star clustersOpen star clusters |
| spellingShingle | R. K. S. Yadav Arvind K. Dattatrey Geeta Rangwal Annapurni Subramaniam D. Bisht Ram Sagar UOCS. XIII. Study of the Far-ultraviolet Bright Stars in the Open Cluster NGC 2420 Using AstroSat The Astrophysical Journal Star clusters Open star clusters |
| title | UOCS. XIII. Study of the Far-ultraviolet Bright Stars in the Open Cluster NGC 2420 Using AstroSat |
| title_full | UOCS. XIII. Study of the Far-ultraviolet Bright Stars in the Open Cluster NGC 2420 Using AstroSat |
| title_fullStr | UOCS. XIII. Study of the Far-ultraviolet Bright Stars in the Open Cluster NGC 2420 Using AstroSat |
| title_full_unstemmed | UOCS. XIII. Study of the Far-ultraviolet Bright Stars in the Open Cluster NGC 2420 Using AstroSat |
| title_short | UOCS. XIII. Study of the Far-ultraviolet Bright Stars in the Open Cluster NGC 2420 Using AstroSat |
| title_sort | uocs xiii study of the far ultraviolet bright stars in the open cluster ngc 2420 using astrosat |
| topic | Star clusters Open star clusters |
| url | https://doi.org/10.3847/1538-4357/ad13e8 |
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