Saved in:
| Main Authors: | , , |
|---|---|
| Format: | Preprint |
| Published: |
2025
|
| Subjects: | |
| Online Access: | https://arxiv.org/abs/2504.10599 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866908319986221056 |
|---|---|
| author | Sheikhnezami, Somayeh Fendt, Christian Ataiee, Sareh |
| author_facet | Sheikhnezami, Somayeh Fendt, Christian Ataiee, Sareh |
| contents | We study the launching of magnetized jets from a resistive circumstellar disk within a binary system, employing a unique combination of 3D MHD jet launching simulations (PLUTO code) and post-processed 3D radiative transfer modeling (RADMC-3D code). Our findings reveal a well-defined jet originating from the inner region of the disk, extending to a larger disk area. While the model attains steady states for a single star, a binary system leads to the emergence of tidal effects such as the formation of ``spiral arms'' in the disk and inside the jet. Here we have consistently implemented a time-dependent Roche potential for the gravity of the binary. As a major step forward, we further present the first 3D radiation maps of the dust continuum for the disk-jet structure. In principle, this allows us to compare MHD simulation results to observed disk-outflow features. We, therefore, present convolved images of the dust continuum emission, employing exemplary point spread functions of the MIRI instrument (5~$μm$ band) and the ALMA array (320~$μm$ band). In these bands, we identify distinguishable features of the disk-jet structure, such as "spiral arms," which we have also seen in the MHD dynamics.For gas density increased by an order of magnitude, the disk become optically thick at 5~$μm$, but remains bright at 320~$μ$m. At this wavelength, 320~$μ$m, enhanced structural features in the disk and the base of the wind become more pronounced and are well resolved in the convolved image. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_10599 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Dust continuum radiation maps from MHD simulations of accretion-ejection systems around single and binary stars Sheikhnezami, Somayeh Fendt, Christian Ataiee, Sareh High Energy Astrophysical Phenomena Solar and Stellar Astrophysics We study the launching of magnetized jets from a resistive circumstellar disk within a binary system, employing a unique combination of 3D MHD jet launching simulations (PLUTO code) and post-processed 3D radiative transfer modeling (RADMC-3D code). Our findings reveal a well-defined jet originating from the inner region of the disk, extending to a larger disk area. While the model attains steady states for a single star, a binary system leads to the emergence of tidal effects such as the formation of ``spiral arms'' in the disk and inside the jet. Here we have consistently implemented a time-dependent Roche potential for the gravity of the binary. As a major step forward, we further present the first 3D radiation maps of the dust continuum for the disk-jet structure. In principle, this allows us to compare MHD simulation results to observed disk-outflow features. We, therefore, present convolved images of the dust continuum emission, employing exemplary point spread functions of the MIRI instrument (5~$μm$ band) and the ALMA array (320~$μm$ band). In these bands, we identify distinguishable features of the disk-jet structure, such as "spiral arms," which we have also seen in the MHD dynamics.For gas density increased by an order of magnitude, the disk become optically thick at 5~$μm$, but remains bright at 320~$μ$m. At this wavelength, 320~$μ$m, enhanced structural features in the disk and the base of the wind become more pronounced and are well resolved in the convolved image. |
| title | Dust continuum radiation maps from MHD simulations of accretion-ejection systems around single and binary stars |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2504.10599 |