%0 Generic %1 vijayaraghavan2017evaporation %A Vijayaraghavan, Rukmani %A Sarazin, Craig %D 2017 %K conduction pressure ram stripping tails thermal %T The Evaporation and Survival of Cluster Galaxies' Coronae Part II: The Effectiveness of Anisotropic Thermal Conduction and Survival of Stripped Galactic Tails %U http://arxiv.org/abs/1706.00021 %X We simulate and characterize the effects of anisotropic thermal conduction between the intracluster medium (ICM) and the hot coronal interstellar medium (ISM) gas in cluster galaxies. In the earlier Paper I (Vijayaraghavan & Sarazin 2017a), we simulated the evaporation of the hot ISM due to isotropic conduction between the ISM and ICM. We found that hot coronae evaporate on $\sim$ $10^2$ Myr timescales, significantly shorter than the $\sim$ $10^3$ Myr gas loss times due to ram pressure stripping. No tails of stripped gas are formed. This is in tension with the observed ubiquity and implied longevity of compact X-ray emitting coronae and stripped ISM tails, and requires the suppression of evaporation due to thermal conduction. ICM magnetic fields restrict the flow of heat from the ICM to the ISM by forcing thermal conduction to be anisotropic, i.e., restricted to directions parallel to the magnetic field. We perform a series of wind tunnel simulations with galaxy and ICM properties identical to the simulations in Paper I, now including ISM and ICM magnetic fields. We simulate a range of extreme magnetic field configurations: parallel and perpendicular to the ICM wind, and continuous and completely disjoint between the ISM and ICM. We perform simulations with and without anisotropic conduction for each magnetic field configuration. We find that magnetic fields and anisotropic conduction severely reduce the gas loss due to thermal evaporation, and the overall gas loss rates with and without anisotropic conduction do not differ by more than $10 - 20\%$. Magnetic fields also prevent stripped tails from evaporating in the ICM by shielding them, and providing few pathways for heat transport between the ICM and ISM. The morphology of stripped tails and magnetic fields in the tails and wakes of galaxies are sensitive to the initial magnetic field configuration.

@misc{vijayaraghavan2017evaporation, abstract = {We simulate and characterize the effects of anisotropic thermal conduction between the intracluster medium (ICM) and the hot coronal interstellar medium (ISM) gas in cluster galaxies. In the earlier Paper I (Vijayaraghavan & Sarazin 2017a), we simulated the evaporation of the hot ISM due to isotropic conduction between the ISM and ICM. We found that hot coronae evaporate on $\sim$ $10^2$ Myr timescales, significantly shorter than the $\sim$ $10^3$ Myr gas loss times due to ram pressure stripping. No tails of stripped gas are formed. This is in tension with the observed ubiquity and implied longevity of compact X-ray emitting coronae and stripped ISM tails, and requires the suppression of evaporation due to thermal conduction. ICM magnetic fields restrict the flow of heat from the ICM to the ISM by forcing thermal conduction to be anisotropic, i.e., restricted to directions parallel to the magnetic field. We perform a series of wind tunnel simulations with galaxy and ICM properties identical to the simulations in Paper I, now including ISM and ICM magnetic fields. We simulate a range of extreme magnetic field configurations: parallel and perpendicular to the ICM wind, and continuous and completely disjoint between the ISM and ICM. We perform simulations with and without anisotropic conduction for each magnetic field configuration. We find that magnetic fields and anisotropic conduction severely reduce the gas loss due to thermal evaporation, and the overall gas loss rates with and without anisotropic conduction do not differ by more than $10 - 20\%$. Magnetic fields also prevent stripped tails from evaporating in the ICM by shielding them, and providing few pathways for heat transport between the ICM and ISM. The morphology of stripped tails and magnetic fields in the tails and wakes of galaxies are sensitive to the initial magnetic field configuration.}, added-at = {2017-06-02T09:55:40.000+0200}, author = {Vijayaraghavan, Rukmani and Sarazin, Craig}, biburl = {https://www.bibsonomy.org/bibtex/20a9c208fc76347ac42ebfd992901e56e/miki}, description = {[1706.00021] The Evaporation and Survival of Cluster Galaxies' Coronae Part II: The Effectiveness of Anisotropic Thermal Conduction and Survival of Stripped Galactic Tails}, interhash = {1631d76cf72f913f470f5ec385c92632}, intrahash = {0a9c208fc76347ac42ebfd992901e56e}, keywords = {conduction pressure ram stripping tails thermal}, note = {cite arxiv:1706.00021Comment: Submitted to ApJ. 23 pages, 14 figures. Animations for this paper are at this URL: https://virginia.app.box.com/v/anisotropic-conduction}, timestamp = {2017-06-02T09:55:40.000+0200}, title = {The Evaporation and Survival of Cluster Galaxies' Coronae Part II: The Effectiveness of Anisotropic Thermal Conduction and Survival of Stripped Galactic Tails}, url = {http://arxiv.org/abs/1706.00021}, year = 2017 }