The Fragmentation Criteria in Local Vertically Stratified Self-gravitating Disk Simulations
Massive circumstellar disks are prone to gravitational instabilities, which trigger the formation of spiral arms that can fragment into bound clumps under the right conditions. Two-dimensional simulations of self-gravitating disks are useful starting points for studying fragmentation because they al...
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ndltd-arizona.edu-oai-arizona.openrepository.com-10150-6261822017-12-06T03:00:35Z The Fragmentation Criteria in Local Vertically Stratified Self-gravitating Disk Simulations Baehr, Hans Klahr, Hubert Kratter, Kaitlin M. Univ Arizona, Steward Observ hydrodynamics instabilities planets and satellites: formation planets and satellites: gaseous planets protoplanetary disks Massive circumstellar disks are prone to gravitational instabilities, which trigger the formation of spiral arms that can fragment into bound clumps under the right conditions. Two-dimensional simulations of self-gravitating disks are useful starting points for studying fragmentation because they allow high-resolution simulations of thin disks. However, convergence issues can arise in 2D from various sources. One of these sources is the 2D approximation of self-gravity, which exaggerates the effect of self-gravity on small scales when the potential is not smoothed to account for the assumed vertical extent of the disk. This effect is enhanced by increased resolution, resulting in fragmentation at longer cooling timescales beta. If true, it suggests that the 3D simulations of disk fragmentation may not have the same convergence problem and could be used to examine the nature of fragmentation without smoothing self-gravity on scales similar to the disk scale height. To that end, we have carried out local 3D self-gravitating disk simulations with simple beta cooling with fixed background irradiation to determine if 3D is necessary to properly describe disk fragmentation. Above a resolution of similar to 40 grid cells per scale height, we find that our simulations converge with respect to the cooling timescale. This result converges in agreement with analytic expectations which place a fragmentation boundary at beta(crit) = 3. 2017-10-09 Article The Fragmentation Criteria in Local Vertically Stratified Self-gravitating Disk Simulations 2017, 848 (1):40 The Astrophysical Journal 1538-4357 10.3847/1538-4357/aa8a66 http://hdl.handle.net/10150/626182 http://arizona.openrepository.com/arizona/handle/10150/626182 The Astrophysical Journal en http://stacks.iop.org/0004-637X/848/i=1/a=40?key=crossref.09720af13744057154f36314debe267a © 2017. The American Astronomical Society. All rights reserved. IOP PUBLISHING LTD |
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en |
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hydrodynamics instabilities planets and satellites: formation planets and satellites: gaseous planets protoplanetary disks |
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hydrodynamics instabilities planets and satellites: formation planets and satellites: gaseous planets protoplanetary disks Baehr, Hans Klahr, Hubert Kratter, Kaitlin M. The Fragmentation Criteria in Local Vertically Stratified Self-gravitating Disk Simulations |
description |
Massive circumstellar disks are prone to gravitational instabilities, which trigger the formation of spiral arms that can fragment into bound clumps under the right conditions. Two-dimensional simulations of self-gravitating disks are useful starting points for studying fragmentation because they allow high-resolution simulations of thin disks. However, convergence issues can arise in 2D from various sources. One of these sources is the 2D approximation of self-gravity, which exaggerates the effect of self-gravity on small scales when the potential is not smoothed to account for the assumed vertical extent of the disk. This effect is enhanced by increased resolution, resulting in fragmentation at longer cooling timescales beta. If true, it suggests that the 3D simulations of disk fragmentation may not have the same convergence problem and could be used to examine the nature of fragmentation without smoothing self-gravity on scales similar to the disk scale height. To that end, we have carried out local 3D self-gravitating disk simulations with simple beta cooling with fixed background irradiation to determine if 3D is necessary to properly describe disk fragmentation. Above a resolution of similar to 40 grid cells per scale height, we find that our simulations converge with respect to the cooling timescale. This result converges in agreement with analytic expectations which place a fragmentation boundary at beta(crit) = 3. |
author2 |
Univ Arizona, Steward Observ |
author_facet |
Univ Arizona, Steward Observ Baehr, Hans Klahr, Hubert Kratter, Kaitlin M. |
author |
Baehr, Hans Klahr, Hubert Kratter, Kaitlin M. |
author_sort |
Baehr, Hans |
title |
The Fragmentation Criteria in Local Vertically Stratified Self-gravitating Disk Simulations |
title_short |
The Fragmentation Criteria in Local Vertically Stratified Self-gravitating Disk Simulations |
title_full |
The Fragmentation Criteria in Local Vertically Stratified Self-gravitating Disk Simulations |
title_fullStr |
The Fragmentation Criteria in Local Vertically Stratified Self-gravitating Disk Simulations |
title_full_unstemmed |
The Fragmentation Criteria in Local Vertically Stratified Self-gravitating Disk Simulations |
title_sort |
fragmentation criteria in local vertically stratified self-gravitating disk simulations |
publisher |
IOP PUBLISHING LTD |
publishDate |
2017 |
url |
http://hdl.handle.net/10150/626182 http://arizona.openrepository.com/arizona/handle/10150/626182 |
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