Absolute Parameters of Young Stars: NO Puppis
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| Autores principales: | , , , , , , , , |
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| Formato: | Preprint |
| Publicado: |
2025
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| author | Erdem, Ahmet Bakış, Volkan Southworth, John Rhodes, Michael D. Aliçavuş, Filiz Kahraman Budding, Edwin Blackford, Mark Banks, Timothy Alexander, Murray |
| author_facet | Erdem, Ahmet Bakış, Volkan Southworth, John Rhodes, Michael D. Aliçavuş, Filiz Kahraman Budding, Edwin Blackford, Mark Banks, Timothy Alexander, Murray |
| contents | The southern early-type, young, eccentric-orbit eclipsing binary NO Puppis forms the A component of the multiple star Gaia DR3 552\-8147999779517568. The B component is an astrometric binary now at a separation of about 8.1 arcsec. There may be other fainter stars in this interesting but complex stellar system. We have combined several lines of evidence, including TESS data from 4 sectors, new ground-based BVR photometry, HARPS (ESO) and HERCULES (UCMJO) high-resolution spectra and astrometry of NO Pup. We derive a revised set of absolute parameters with increased precision. Alternative optimal curve-fitting programs were used in the analysis, allowing a wider view of modelling and parameter uncertainties. The main parameters are as follows: $M_{Aa} = 3.58 \pm 0.11$, $M_{Ab} = 1.68 \pm 0.09$ (M$_\odot$); $R_{Aa} = 2.17 \pm 0.03$, $R_{Ab} = 1.51 \pm 0.06$ (R$_\odot$), and $T_{\rm e Aa} = 13300 \pm 500$, $T_{\rm e Ab} = 7400 \pm 500$ (K). We estimate approximate masses of the wide companions, Ba and Bb, as $M_{Ba} = 2.0$ and $M_{Bb} = 1.8$ (M$_\odot$). The close binary's orbital separation is $a= 8.51 \pm 0.05$ (R$_\odot$); its age is approximately $20$ Myr and distance $172 \pm 1$ pc. The close binary's secondary (Ab) appears to be the source of low amplitude $ δ$ Scuti-type oscillations, although the form of these oscillations is irregular and unrepetitive. Analysis of the $ λ$ 6678 He I profile of the primary show synchronism of the mean bodily and orbital rotations. The retention of significant orbital eccentricity, in view of the closeness of the A-system components, is unexpected and poses challenges for the explanation that we discuss. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_05893 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Absolute Parameters of Young Stars: NO Puppis Erdem, Ahmet Bakış, Volkan Southworth, John Rhodes, Michael D. Aliçavuş, Filiz Kahraman Budding, Edwin Blackford, Mark Banks, Timothy Alexander, Murray Solar and Stellar Astrophysics The southern early-type, young, eccentric-orbit eclipsing binary NO Puppis forms the A component of the multiple star Gaia DR3 552\-8147999779517568. The B component is an astrometric binary now at a separation of about 8.1 arcsec. There may be other fainter stars in this interesting but complex stellar system. We have combined several lines of evidence, including TESS data from 4 sectors, new ground-based BVR photometry, HARPS (ESO) and HERCULES (UCMJO) high-resolution spectra and astrometry of NO Pup. We derive a revised set of absolute parameters with increased precision. Alternative optimal curve-fitting programs were used in the analysis, allowing a wider view of modelling and parameter uncertainties. The main parameters are as follows: $M_{Aa} = 3.58 \pm 0.11$, $M_{Ab} = 1.68 \pm 0.09$ (M$_\odot$); $R_{Aa} = 2.17 \pm 0.03$, $R_{Ab} = 1.51 \pm 0.06$ (R$_\odot$), and $T_{\rm e Aa} = 13300 \pm 500$, $T_{\rm e Ab} = 7400 \pm 500$ (K). We estimate approximate masses of the wide companions, Ba and Bb, as $M_{Ba} = 2.0$ and $M_{Bb} = 1.8$ (M$_\odot$). The close binary's orbital separation is $a= 8.51 \pm 0.05$ (R$_\odot$); its age is approximately $20$ Myr and distance $172 \pm 1$ pc. The close binary's secondary (Ab) appears to be the source of low amplitude $ δ$ Scuti-type oscillations, although the form of these oscillations is irregular and unrepetitive. Analysis of the $ λ$ 6678 He I profile of the primary show synchronism of the mean bodily and orbital rotations. The retention of significant orbital eccentricity, in view of the closeness of the A-system components, is unexpected and poses challenges for the explanation that we discuss. |
| title | Absolute Parameters of Young Stars: NO Puppis |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2508.05893 |