Binary Parameters for the Recurrent Nova T Coronae Borealis
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arXiv
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| Autori principali: | , , , , , |
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| Natura: | Preprint |
| Pubblicazione: |
2025
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| _version_ | 1866916635040808960 |
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| author | Hinkle, Kenneth H. Nagarajan, Pranav Fekel, Francis C. Mikołajewska, Joanna Straniero, Oscar Muterspaugh, Matthew W. |
| author_facet | Hinkle, Kenneth H. Nagarajan, Pranav Fekel, Francis C. Mikołajewska, Joanna Straniero, Oscar Muterspaugh, Matthew W. |
| contents | T CrB is among the brightest novae. It is recurrent with outbursts happening approximately every 80 years. The next outburst is imminent, expected in 2025. The T CrB binary consists of an M4 III red giant (RG) secondary and a white dwarf (WD) primary. A time series of spectra of the RG was obtained between 2022 and 2024. Radial velocities (RVs) from these data were combined with literature RVs and an updated orbit computed. The orbit is circular to a high precision and has a period of 227.5494 +/- 0.0049 days for the circular solution. An eccentric solution yields an eccentricity of 0.0072 +/- 0.0026. Rotational line broadening of the RG was also measured. Binary parameters are derived by maximum likelihood modeling of the available observational data. The WD, in accord with other estimates for recurrent novae, is massive. Assuming the Gaia distance, the WD mass is 1.37 +/- 0.01 M sun with the M giant secondary mass 0.69 +0.02/-0.01 M sun. We discuss the evolution of this system and both paths to and limitations on further refining the values of the system parameters. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2502_20664 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Binary Parameters for the Recurrent Nova T Coronae Borealis Hinkle, Kenneth H. Nagarajan, Pranav Fekel, Francis C. Mikołajewska, Joanna Straniero, Oscar Muterspaugh, Matthew W. Solar and Stellar Astrophysics T CrB is among the brightest novae. It is recurrent with outbursts happening approximately every 80 years. The next outburst is imminent, expected in 2025. The T CrB binary consists of an M4 III red giant (RG) secondary and a white dwarf (WD) primary. A time series of spectra of the RG was obtained between 2022 and 2024. Radial velocities (RVs) from these data were combined with literature RVs and an updated orbit computed. The orbit is circular to a high precision and has a period of 227.5494 +/- 0.0049 days for the circular solution. An eccentric solution yields an eccentricity of 0.0072 +/- 0.0026. Rotational line broadening of the RG was also measured. Binary parameters are derived by maximum likelihood modeling of the available observational data. The WD, in accord with other estimates for recurrent novae, is massive. Assuming the Gaia distance, the WD mass is 1.37 +/- 0.01 M sun with the M giant secondary mass 0.69 +0.02/-0.01 M sun. We discuss the evolution of this system and both paths to and limitations on further refining the values of the system parameters. |
| title | Binary Parameters for the Recurrent Nova T Coronae Borealis |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2502.20664 |