Results 21 to 30 of about 544 (157)
Turbulence in the intragroup and circumgalactic medium [PDF]
Astronomy & Astrophysics, 2021 Context. In massive objects, such as galaxy clusters, the turbulent velocity dispersion, σturb, is tightly correlated to both the object mass, M, and the thermal energy. Aims. Here, we investigate whether these scaling laws extend to lower-mass objects in dark-matter filaments. Methods.
Schmidt, W., Schmidt, J. P., Grete, P.
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Efficiency of thermal conduction in a magnetized circumgalactic medium [PDF]
Monthly Notices of the Royal Astronomical Society, 2021 ABSTRACT The large temperature difference between cold gas clouds around galaxies and the hot haloes that they are moving through suggests that thermal conduction could play an important role in the circumgalactic medium. However, thermal conduction in the presence of a magnetic field is highly anisotropic, being strongly suppressed in ...
Richard Kooij +2 more
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The circumgalactic medium of high-redshift galaxies [PDF]
Monthly Notices of the Royal Astronomical Society: Letters, 2014 Abstract We study the properties of the circumgalactic medium (CGM) of high-z galaxies in the metal enrichment simulations presented in Pallottini et al. At z = 4, we find that the simulated CGM gas density profiles are self-similar, once scaled with the virial radius of the parent dark matter halo.
PALLOTTINI, ANDREA +2 more
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Role of cosmic rays in the circumgalactic medium [PDF]
Monthly Notices of the Royal Astronomical Society, 2015 We explore the impact of cosmic rays (CRs) on cosmological adaptive-mesh refinement simulations of a forming 10^12 Msolar halo, focusing on the circumgalactic medium (CGM), and its resulting low-redshift structure and composition. In contrast to a run with star formation and energetic feedback but no CRs, the CR-inclusive runs feature a CGM ...
Salem, Munier +2 more
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The origins of the circumgalactic medium in the FIRE simulations [PDF]
Monthly Notices of the Royal Astronomical Society, 2019 ABSTRACT We use a particle tracking analysis to study the origins of the circumgalactic medium (CGM), separating it into (1) accretion from the intergalactic medium (IGM), (2) wind from the central galaxy, and (3) gas ejected from other galaxies. Our sample consists of 21 FIRE-2 simulations, spanning the halo mass range Mh ∼ 1010–1012 M⊙,
Norman Murray +12 more
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The Circumgalactic Medium of Andromeda [PDF]
Proceedings of the International Astronomical Union, 2016 AbstractOur view of galaxies has been transformed in recent years with diffuse halo gas surrounding galaxies that contains at least as many metals and baryons as their disks. While single sight lines through galaxy halos seen in absorption have provided key new constraints, they provide only average properties. Our massive neighbor, the Andromeda (M31)
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The impact of galactic feedback on the circumgalactic medium [PDF]
Monthly Notices of the Royal Astronomical Society, 2015 17 pages, 12 figures, accepted to ...
Suresh, Joshua +7 more
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Cosmic Ray Processes in Galactic Ecosystems
Galaxies, 2023 Galaxy evolution is an important topic, and our physical understanding must be complete to establish a correct picture. This includes a thorough treatment of feedback.
Ellis R. Owen +4 more
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The Circumgalactic Medium of Quasars [PDF]
Proceedings of the International Astronomical Union, 2013 AbstractI will argue that observations of the diffuse gas in the outskirts of quasar host galaxies, or the so called circumgalactic medium, are essential for understanding how luminous quasars evolve in a cosmological context. Such observations also provide a fruitful comparison to theory, because hydrodynamics at moderate overdensities is much easier ...
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Formation of multiphase plasma in galactic haloes and an analogy to solar plasma
Frontiers in Astronomy and Space Sciences, 2023 Thermal instability (TI) potentially explains the origin of cold gas in the intracluster medium (ICM), which is heated sufficiently by AGN feedback. The Hα filaments seen in cluster cores provide strong motivation for TI.
Prakriti Pal Choudhury
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