Evidence for an accretion bridge in the DX Cha circumbinary system from VLTI/MATISSE observations
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| Format: | Preprint |
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2025
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| _version_ | 1866910831722102784 |
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| author | Juhász, Tímea Varga, József Ábrahám, Péter Kóspál, Ágnes Lykou, Foteini Chen, Lei Moór, Attila de Miera, Fernando Cruz-Sáenz Lopez, Bruno Matter, Alexis van Boekel, Roy Hogerheijde, Michiel Abello, Margaux Augereau, Jean-Charles Boley, Paul Danchi, William C. Henning, Thomas Letessier, Mathis Ma, Jie Priolet, Philippe Scheuck, Marten Weigelt, Gerd Wolf, Sebastian |
| author_facet | Juhász, Tímea Varga, József Ábrahám, Péter Kóspál, Ágnes Lykou, Foteini Chen, Lei Moór, Attila de Miera, Fernando Cruz-Sáenz Lopez, Bruno Matter, Alexis van Boekel, Roy Hogerheijde, Michiel Abello, Margaux Augereau, Jean-Charles Boley, Paul Danchi, William C. Henning, Thomas Letessier, Mathis Ma, Jie Priolet, Philippe Scheuck, Marten Weigelt, Gerd Wolf, Sebastian |
| contents | DX Cha (HD 104237) is a spectroscopic binary consisting of a Herbig A7.5Ve-A8Ve primary star and a K3-type companion. Here we report on new $3.55$ micrometer interferometric observations of this source with the Multi Aperture Mid-Infrared Spectroscopic Experiment (MATISSE) at the Very Large Telescope Interferometer (VLTI). To model the four MATISSE observations obtained between 2020 and 2023, we constructed a time-dependent interferometric model of the system, using the oimodeler software. The model consists of an asymmetric ring and two point sources on a Keplerian orbit. Our best-fit model consists of a circumbinary ring with a diameter of $0.86$ au ($8.1$ mas), featuring a strong azimuthal asymmetry. We found that the position angle of the asymmetry changes tens of degrees between the MATISSE epochs. The ring is relatively narrow, with a full width at half maximum (FWHM) of $\sim$$0.13$ au ($1.23$ mas). The presence of circumstellar dust emission so close to the binary is unexpected, as previous hydrodynamic simulations predicted an inner disk cavity with a diameter of $\sim$$4$ au ($\sim$$37.5$ mas). Thus, we argue that the narrow envelope of material we detected is probably not a gravitationally stable circumbinary ring, but may be part of tidal accretion streamers channeling material from the inner edge of the disk toward the stars. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2502_11722 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Evidence for an accretion bridge in the DX Cha circumbinary system from VLTI/MATISSE observations Juhász, Tímea Varga, József Ábrahám, Péter Kóspál, Ágnes Lykou, Foteini Chen, Lei Moór, Attila de Miera, Fernando Cruz-Sáenz Lopez, Bruno Matter, Alexis van Boekel, Roy Hogerheijde, Michiel Abello, Margaux Augereau, Jean-Charles Boley, Paul Danchi, William C. Henning, Thomas Letessier, Mathis Ma, Jie Priolet, Philippe Scheuck, Marten Weigelt, Gerd Wolf, Sebastian Solar and Stellar Astrophysics Earth and Planetary Astrophysics Astrophysics of Galaxies DX Cha (HD 104237) is a spectroscopic binary consisting of a Herbig A7.5Ve-A8Ve primary star and a K3-type companion. Here we report on new $3.55$ micrometer interferometric observations of this source with the Multi Aperture Mid-Infrared Spectroscopic Experiment (MATISSE) at the Very Large Telescope Interferometer (VLTI). To model the four MATISSE observations obtained between 2020 and 2023, we constructed a time-dependent interferometric model of the system, using the oimodeler software. The model consists of an asymmetric ring and two point sources on a Keplerian orbit. Our best-fit model consists of a circumbinary ring with a diameter of $0.86$ au ($8.1$ mas), featuring a strong azimuthal asymmetry. We found that the position angle of the asymmetry changes tens of degrees between the MATISSE epochs. The ring is relatively narrow, with a full width at half maximum (FWHM) of $\sim$$0.13$ au ($1.23$ mas). The presence of circumstellar dust emission so close to the binary is unexpected, as previous hydrodynamic simulations predicted an inner disk cavity with a diameter of $\sim$$4$ au ($\sim$$37.5$ mas). Thus, we argue that the narrow envelope of material we detected is probably not a gravitationally stable circumbinary ring, but may be part of tidal accretion streamers channeling material from the inner edge of the disk toward the stars. |
| title | Evidence for an accretion bridge in the DX Cha circumbinary system from VLTI/MATISSE observations |
| topic | Solar and Stellar Astrophysics Earth and Planetary Astrophysics Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2502.11722 |