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| Autore principale: | |
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| Natura: | Preprint |
| Pubblicazione: |
2026
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| Soggetti: | |
| Accesso online: | https://arxiv.org/abs/2601.00718 |
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| _version_ | 1866909980004712448 |
|---|---|
| author | Stȩpień, K. |
| author_facet | Stȩpień, K. |
| contents | A comprehensive evolution study was conducted on a carefully
selected sample of near-contact binaries (NCBs) with more massive
components filling the Roche lobes, utilizing the best-known basic
parameters and indications of ongoing mass transfer. The results and
discussion highlight that several NCBs with total masses exceeding 2 solar masses
survive only a short time after mass exchange as contact binaries (CBs),
with both components eventually merging to form a rapidly rotating giant,
akin to FK~Com. Less massive NCBs transition into typical CBs and
remain in this phase for up to 2 Gyr before ending their binary evolution
as systems with extremely low mass ratios, susceptible to Darwin
instability.
However, this does not fully explain the existence of low-mass CBs with
masses in the range of 1-1.5 solar masses. It is noted that there exists a
population of low-mass binaries, nearly filling their Roche lobes. Their
overall properties suggest that they could be progenitors of low-mass
CBs. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2601_00718 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Near-Contact Binaries on the Path to Contact Binaries Stȩpień, K. Solar and Stellar Astrophysics A comprehensive evolution study was conducted on a carefully selected sample of near-contact binaries (NCBs) with more massive components filling the Roche lobes, utilizing the best-known basic parameters and indications of ongoing mass transfer. The results and discussion highlight that several NCBs with total masses exceeding 2 solar masses survive only a short time after mass exchange as contact binaries (CBs), with both components eventually merging to form a rapidly rotating giant, akin to FK~Com. Less massive NCBs transition into typical CBs and remain in this phase for up to 2 Gyr before ending their binary evolution as systems with extremely low mass ratios, susceptible to Darwin instability. However, this does not fully explain the existence of low-mass CBs with masses in the range of 1-1.5 solar masses. It is noted that there exists a population of low-mass binaries, nearly filling their Roche lobes. Their overall properties suggest that they could be progenitors of low-mass CBs. |
| title | Near-Contact Binaries on the Path to Contact Binaries |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2601.00718 |