Results 51 to 60 of about 889,569 (256)
The Structure of an 80 Parsec Long Massive Filament
The Astronomical JournalUsing new Institut de Radioastronomie Millimétrique 30 m telescope N _2 H ^+ , C ^18 O J = 1–0 and Atacama Pathfinder Experiment telescope ^13 CO and C ^18 O J = 2–1 maps together with archival far-infrared continuum data, and ^12 CO, and ^13 CO J = 1–
Qian-Ru He +13 more
doaj +1 more source
THE IMPLICATIONS OF A HIGH COSMIC-RAY IONIZATION RATE IN DIFFUSE INTERSTELLAR CLOUDS [PDF]
, 2009 Diffuse interstellar clouds show large abundances of H+3 which can only be maintained by a high ionization rate of H2. Cosmic rays are the dominant ionization mechanism in this environment, so the large ionization rate implies a high cosmic-ray flux, and
N. Indriolo +2 more
semanticscholar +1 more source
ON THE DENSITY DISTRIBUTION IN STAR-FORMING INTERSTELLAR CLOUDS [PDF]
TeraGrid Conference, 2010 We use deep adaptive mesh refinement simulations of isothermal self-gravitating supersonic turbulence to study the imprints of gravity on the mass density distribution in molecular clouds.
A. Kritsuk, M. Norman, Rick Wagner
semanticscholar +1 more source
Interstellar Scintillation and Clouds of the Interstellar Turbulent Plasma [PDF]
International Astronomical Union Colloquium, 2001 AbstractData on interstellar diffraction and refraction scintillation of pulsars are analyzed. Comparison between theory and the observational data shows that two types of spectra for electron density fluctuations are realized in the interstellar medium: pure power law and piecewise with a break. The distribution of turbulent plasma in the Galaxy has a
openaire +2 more sources
Tidal Disruption of “Snow Clouds” by Unassociated Stars
The Astrophysical JournalIt has been suggested that star-forming galaxies may host a substantial, dark reservoir of gas in the form of planetary-mass molecular clouds that are so cold that H _2 can condense.
Arthur G. Suvorov, Mark A. Walker
doaj +1 more source
Frontiers in Astronomy and Space Sciences, 2023 Combined in situ observations of the interstellar wind through the solar system and of its pickup ions (PUIs), implanted after ionization in the solar wind, explain, in comparison with interstellar absorption lines of nearby stars, that the Sun is in an ...
Eberhard Möbius
doaj +1 more source
Two-component model of the interaction of an interstellar cloud with surrounding hot plasma
, 2011 We present a two-component gasdynamic model of an interstellar cloud embedded in a hot plasma. It is assumed that the cloud consists of atomic hydrogen gas, interstellar plasma is quasineutral.
Baranov +23 more
core +2 more sources
On the structure of the turbulent interstellar clouds . Influence of the equation of state on the dynamics of 3D compressible flows [PDF]
, 2009 Context. It is well established that the atomic interstellar hydrogen is filling the galaxies and constitutes the building blocks of molecular clouds. Aims. To understand the formation and the evolution of molecular clouds, it is necessary to investigate
E. Audit, P. Hennebelle
semanticscholar +1 more source
Formation of interstellar clouds: Parker instability with phase transitions [PDF]
, 2009 We numerically follow the nonlinear evolution of the Parker instability in the presence of phase transitions from a warm to a cold H i interstellar medium in two spatial dimensions.
T. Mouschovias, M. Kunz, D. Christie
semanticscholar +1 more source
Valence Threshold Photoionization Spectra of C5$_5$H and C5$_5$H2$_2$ Isomers
ChemPhysChem, Volume 27, Issue 8, 28 April 2026.Mass‐selected threshold photoelectron spectra (TPES) of l‐C5H, HC5H, and c–C3H‐CCH were recorded using double‐imaging photoelectron‐photoion coincidence spectroscopy. These transient species were generated in situ by hydrogen abstraction from cyclopropylacetylene and 1,3‐pentadiyne.
Ugo Jacovella +9 more
wiley +1 more source