![]() Represents a gaseous, multiphase plasma surrounding the The circumgalactic medium (CGM) of the Milky Way (MW) Which point toward a strong interaction between the LMC’s Velocity components, the faster among them being possiblyĮxtraplanar (Luks & Rohlfs 1992 Nidever et al. The leading edge is characterized by multiple HI (van der Marel & Cioni 2001), which would rule out a tidalĮxplanation for this HI truncation (as tides would truncate both Stellar profile continues uninterrupted well beyond this radius (see Section 2.1), in contrast to other quadrants of the LMC Hereafter as its “leading edge.” The HI profile here truncatesĪbruptly at R » 6.2 kpc from the kinematic center of the LMC Most directly impact the disk’s northeastern edge, referred to Motion (PM) vector implies that any CGM headwind would Of this complex with the CGM likely alters the appearance andĭynamics of these gaseous components. Of gas strewn across much of the southern sky. With a Leading Arm (LA) and trailing Magellanic Stream (MS) The Magellanic Clouds (MCs) move through the MWĪt ∼50 kpc from the Galactic Center at velocities ∼300 km s−1, Stellar disks and well-constrained orbital properties. Paper we instead consider the Large Magellanic Cloud (LMC),Ī relatively massive, late-type dwarf, with well-studied HI and To place preliminary bounds on the CGM’s gas profile. Host of dwarf spheroidals orbiting the MW, most devoid of HI, Grcevich & Putman (2009) and Gatto et al. Temperature (e.g., Roediger & Hensler 2005, find only a slightĭependence on the Mach number of the flow). The stripping dynamics are insensitive to the oncoming wind’s Probe diffuse gas of all temperatures and ionization states, and In contrast, studies that exploit ram pressure stripping (RPS) Photoionization a single waveband study cannot probe theīroad range of gas phases spanned by the CGM in all its forms. Key words: Galaxy: structure – hydrodynamics – intergalactic medium – Magellanic Clouds Mass M (300 kpc) = 2.7 1.4 ´ 1010M or approximately 15% of a 1012M MW’s baryonic mass budget. From our work, assuming a β-profile valid to ∼rvir, we infer a total diffuse CGM This result imposes an important constraint on the density profile of the MW’s CGM at 50 kpc, and thus also on the The broader CGM and temperature profiles, thus providing a model-independent constraint on the local gas density. The implied pericentric density proves to be insensitive to both Leading (windward) edge only in scenarios where the MW CGM density at pericentric passage is Our simulations can match the radial extent of the LMC’s ![]() WeĮxplore the implications of this ram pressure stripping signature, using both analytic prescriptions and full threedimensional hydrodynamic simulations of the LMC. Profile along the windward “leading edge” of the LMC disk, despite a far more extended stellar component. From the observed stellar and HI distributions of the system we find evidence of a truncated gas Gaseous disk has recently experienced stripping, suggesting the extent of its HI disk directly probes the medium in Well-constrained pericentric passage about the Milky Way (MW) ∼50 Myr ago. Recent observations have constrained the orbit and structure of the Large Magellanic Cloud (LMC), implying a Received 2015 July 20 accepted 2015 October 29 published 2015 December 10 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, 21218, USAĬarnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA van der Marel3, and Stephanie Tonnesen4ĭepartment of Astronomy, Columbia University, 550 West 120th Street, New York, NY, 10027, USA of Astronomy, University of Arizona, 933 North Cherry Avenue, Tucson, AZ, 85721, USA Munier Salem1, Gurtina Besla2, Greg Bryan1, Mary Putman1, Roeland P. RAM PRESSURE STRIPPING OF THE LARGE MAGELLANIC CLOUD’S DISK AS A PROBE OF THE MILKY ![]() I am aware there is also a Mach-based RR formula and it has the same problem.The Astrophysical Journal, 815:77 (30pp), 2015 December 10 I also can't find any space shuttle telemetry to corroborate the TAS assumptions I made above. So are these RR=TAS²/87 formulas assuming to be used below a specific altitude? I can't find anything for orbit or reentry. which makes no sense because there are practically no molecules of air to hit! Therefore, my TAT (OAT plus ram rise) is in the thousands of degrees Kelvin. They do not appear to take into account the static pressure or atmospheric composition, only the adiabatic index. My assumption is that if I am in orbit say at 120 km altitude with an instantaneous velocity of 8 km/s my TAS would be fairly close to 8 km/s even though my Indicated Airspeed (IAS) shows zero.Īssuming the above holds true, the "ram rise" (RR) formulas I find are all based on Mach (which, in turn, is based on TAS) or TAS directly. True Airspeed (TAS) is the vehicle speed relative to the surrounding air.
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