Magnetized Protoplanetary Disks around Young Stars in the Presence of Realistic Cooling
In this paper, we study the effects of magnetic fields and ohmic resistivity on the structure of protoplanetary disks (PPDs) in the presence of realistic radiative cooling. We use the self-similar method to solve the magnetohydrodynamic equations in spherical coordinates ( r , θ , ϕ ). Our solutio...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ada93f |
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| author | Hanifeh Ghanbarnejad Maryam Ghasemnezhad |
| author_facet | Hanifeh Ghanbarnejad Maryam Ghasemnezhad |
| author_sort | Hanifeh Ghanbarnejad |
| collection | DOAJ |
| description | In this paper, we study the effects of magnetic fields and ohmic resistivity on the structure of protoplanetary disks (PPDs) in the presence of realistic radiative cooling. We use the self-similar method to solve the magnetohydrodynamic equations in spherical coordinates ( r , θ , ϕ ). Our solutions indicate that a strong magnetic field reduces the outflow region while increasing the mass accretion rate, which in turn leads to a thicker disk. Our model applied to the FU Orionis PPD indicates that in the inner regions of the disk ( r = 10 au), $\dot{M}$ is the order of $\dot{M}\approx 5\times 1{0}^{-4}{M}_{\odot }\,{\mathrm{yr}}^{-1}$ and the mass outflow rate is ${\dot{M}}_{w}=0.1{\dot{M}}_{\mathrm{acc}}$ , which is consistent with the observed range of accretion rates. Additionally, we calculated the cooling timescale in our model to assess one possible fragmentation condition necessary for planet formation. Our results indicate that, although the gravitational instability condition exists in the midplane of the disk, the cooling timescale is not short enough ( τ _cool ≈ 1000Ω ^−1 ), and one possible mechanism for planet formation is not met. |
| format | Article |
| id | doaj-art-b570043a16414387976bb32c7ea6a85b |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-b570043a16414387976bb32c7ea6a85b2025-02-12T07:39:38ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01980216610.3847/1538-4357/ada93fMagnetized Protoplanetary Disks around Young Stars in the Presence of Realistic CoolingHanifeh Ghanbarnejad0Maryam Ghasemnezhad1https://orcid.org/0000-0001-8494-5850Department of Interdisciplinary Physics and Technology, Shahid Bahonar University of Kerman , Kerman, Iran ; m.ghasemnezhad@uk.ac.irDepartment of Interdisciplinary Physics and Technology, Shahid Bahonar University of Kerman , Kerman, Iran ; m.ghasemnezhad@uk.ac.irIn this paper, we study the effects of magnetic fields and ohmic resistivity on the structure of protoplanetary disks (PPDs) in the presence of realistic radiative cooling. We use the self-similar method to solve the magnetohydrodynamic equations in spherical coordinates ( r , θ , ϕ ). Our solutions indicate that a strong magnetic field reduces the outflow region while increasing the mass accretion rate, which in turn leads to a thicker disk. Our model applied to the FU Orionis PPD indicates that in the inner regions of the disk ( r = 10 au), $\dot{M}$ is the order of $\dot{M}\approx 5\times 1{0}^{-4}{M}_{\odot }\,{\mathrm{yr}}^{-1}$ and the mass outflow rate is ${\dot{M}}_{w}=0.1{\dot{M}}_{\mathrm{acc}}$ , which is consistent with the observed range of accretion rates. Additionally, we calculated the cooling timescale in our model to assess one possible fragmentation condition necessary for planet formation. Our results indicate that, although the gravitational instability condition exists in the midplane of the disk, the cooling timescale is not short enough ( τ _cool ≈ 1000Ω ^−1 ), and one possible mechanism for planet formation is not met.https://doi.org/10.3847/1538-4357/ada93fProtoplanetary disksProtostarsMagnetic fields |
| spellingShingle | Hanifeh Ghanbarnejad Maryam Ghasemnezhad Magnetized Protoplanetary Disks around Young Stars in the Presence of Realistic Cooling The Astrophysical Journal Protoplanetary disks Protostars Magnetic fields |
| title | Magnetized Protoplanetary Disks around Young Stars in the Presence of Realistic Cooling |
| title_full | Magnetized Protoplanetary Disks around Young Stars in the Presence of Realistic Cooling |
| title_fullStr | Magnetized Protoplanetary Disks around Young Stars in the Presence of Realistic Cooling |
| title_full_unstemmed | Magnetized Protoplanetary Disks around Young Stars in the Presence of Realistic Cooling |
| title_short | Magnetized Protoplanetary Disks around Young Stars in the Presence of Realistic Cooling |
| title_sort | magnetized protoplanetary disks around young stars in the presence of realistic cooling |
| topic | Protoplanetary disks Protostars Magnetic fields |
| url | https://doi.org/10.3847/1538-4357/ada93f |
| work_keys_str_mv | AT hanifehghanbarnejad magnetizedprotoplanetarydisksaroundyoungstarsinthepresenceofrealisticcooling AT maryamghasemnezhad magnetizedprotoplanetarydisksaroundyoungstarsinthepresenceofrealisticcooling |