Correlation between accretion rate and free-free emission in protoplanetary disks -- A multi-wavelength analysis of central mm/cm emission in transition disks
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| Format: | Preprint |
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2024
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| _version_ | 1866917578929078272 |
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| author | Rota, Alessia A. Meijerhof, Jurrian D. van der Marel, Nienke Francis, Logan van der Tak, Floris S. Sellek, Andrew D. |
| author_facet | Rota, Alessia A. Meijerhof, Jurrian D. van der Marel, Nienke Francis, Logan van der Tak, Floris S. Sellek, Andrew D. |
| contents | The inner regions of protoplanetary disks are the locations where most of planets are thought to form and where processes that influence the global evolution of the disk, such as MHD-winds and photoevaporation, originate. Transition disks (TDs) with large inner dust cavities are the ideal targets to study the inner tens of au of disks, as the central emission can be fully disentangled from the outer disk emission. We present a homogeneous multi-wavelength analysis of the continuum emission in a sample of 11 TDs. We investigate the nature of the central emission close to the star, distinguishing between thermal dust and free-free emission. Spatially resolved measurements of continuum emission from archival ALMA data are combined with literature cm-wave observations to study the spectral indices of the inner and outer disks separately. While the emission from the outer disks is consistent with thermal dust emission, 10/11 of the spectral indices estimated for the central emission close to the star suggest that this emission is free-free emission, likely associated with an ionized jet or a disk wind. No correlation between the free-free luminosity and the accretion luminosity or the X-ray luminosity is found, arguing against the photoevaporative wind origin. A sub-linear correlation between the ionized mass loss rate and the accretion rate onto the star is observed, suggesting an origin in an ionized jet. The relative lack of mm-dust grains in the majority of inner disks in transition disks suggests that either such dust grains have drifted quickly towards the central star, grain growth is less efficient in the inner disk, or grains grow rapidly to planetesimal sizes in the inner disk. The observed correlation between the ionized mass loss rate and the accretion rate suggests the outflow is strictly connected with the stellar accretion and that accretion in these disks is driven by a jet. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2401_05798 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Correlation between accretion rate and free-free emission in protoplanetary disks -- A multi-wavelength analysis of central mm/cm emission in transition disks Rota, Alessia A. Meijerhof, Jurrian D. van der Marel, Nienke Francis, Logan van der Tak, Floris S. Sellek, Andrew D. Earth and Planetary Astrophysics Solar and Stellar Astrophysics The inner regions of protoplanetary disks are the locations where most of planets are thought to form and where processes that influence the global evolution of the disk, such as MHD-winds and photoevaporation, originate. Transition disks (TDs) with large inner dust cavities are the ideal targets to study the inner tens of au of disks, as the central emission can be fully disentangled from the outer disk emission. We present a homogeneous multi-wavelength analysis of the continuum emission in a sample of 11 TDs. We investigate the nature of the central emission close to the star, distinguishing between thermal dust and free-free emission. Spatially resolved measurements of continuum emission from archival ALMA data are combined with literature cm-wave observations to study the spectral indices of the inner and outer disks separately. While the emission from the outer disks is consistent with thermal dust emission, 10/11 of the spectral indices estimated for the central emission close to the star suggest that this emission is free-free emission, likely associated with an ionized jet or a disk wind. No correlation between the free-free luminosity and the accretion luminosity or the X-ray luminosity is found, arguing against the photoevaporative wind origin. A sub-linear correlation between the ionized mass loss rate and the accretion rate onto the star is observed, suggesting an origin in an ionized jet. The relative lack of mm-dust grains in the majority of inner disks in transition disks suggests that either such dust grains have drifted quickly towards the central star, grain growth is less efficient in the inner disk, or grains grow rapidly to planetesimal sizes in the inner disk. The observed correlation between the ionized mass loss rate and the accretion rate suggests the outflow is strictly connected with the stellar accretion and that accretion in these disks is driven by a jet. |
| title | Correlation between accretion rate and free-free emission in protoplanetary disks -- A multi-wavelength analysis of central mm/cm emission in transition disks |
| topic | Earth and Planetary Astrophysics Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2401.05798 |