FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W3125968118> ?p ?o ?g. }

• W3125968118 abstract "Context. Efforts to compare polarization measurements with synthetic observations from magnetohydrodynamics (MHD) models have previously concentrated on the scale of molecular clouds.Aims. We extend the model comparisons to kiloparsec scales, taking into account hot shocked gas generated by supernovae and a non-uniform dynamo-generated magnetic field at both large and small scales down to 4 pc spatial resolution.Methods. We used radiative transfer calculations to model dust emission and polarization on top of MHD simulations. We computed synthetic maps of column density N H , polarization fraction p , and polarization angle dispersion S , and studied their dependencies on important properties of MHD simulations. These include the large-scale magnetic field and its orientation, the small-scale magnetic field, and supernova-driven shocks.Results. Similar filament-like structures of S as seen in the Planck all-sky maps are visible in our synthetic results, although the smallest scale structures are absent from our maps. Supernova-driven shock fronts and S do not show significant correlation. Instead, S can clearly be attributed to the distribution of the small-scale magnetic field. We also find that the large-scale magnetic field influences the polarization properties, such that, for a given strength of magnetic fluctuation, a strong plane of the sky mean field weakens the observed S , while strengthening p . The anticorrelation of p and S , and decreasing p as a function of N H are consistent across all synthetic observations. The magnetic fluctuations follow an exponential distribution, rather than Gaussian characteristic of flows with intermittent repetitive shocks.Conclusions. The observed polarization properties and column densities are sensitive to the line-of-sight distance over which the emission is integrated. Studying synthetic maps as the function of maximum integration length will further help with the interpretation of observations. The effects of the large-scale magnetic field orientation on the polarization properties are difficult to be quantified from observations solely, but MHD models might turn out to be useful for separating the effect of the large-scale mean field." @default.
• W3125968118 created "2021-02-01" @default.
• W3125968118 creator A5031629792 @default.
• W3125968118 creator A5042881564 @default.
• W3125968118 creator A5072557695 @default.
• W3125968118 creator A5073540071 @default.
• W3125968118 date "2018-06-01" @default.
• W3125968118 modified "2023-10-18" @default.
• W3125968118 title "The supernova-regulated ISM: IV. A comparison of simulated polarization with Planck observations" @default.
• W3125968118 cites W1603087138 @default.
• W3125968118 cites W1621862116 @default.
• W3125968118 cites W1967311303 @default.
• W3125968118 cites W1969559681 @default.
• W3125968118 cites W1979376942 @default.
• W3125968118 cites W1979793157 @default.
• W3125968118 cites W1982202820 @default.
• W3125968118 cites W1990670394 @default.
• W3125968118 cites W1991774381 @default.
• W3125968118 cites W2000586963 @default.
• W3125968118 cites W2001530733 @default.
• W3125968118 cites W2009802717 @default.
• W3125968118 cites W2020913145 @default.
• W3125968118 cites W2023806734 @default.
• W3125968118 cites W2025043891 @default.
• W3125968118 cites W2027055131 @default.
• W3125968118 cites W2028408599 @default.
• W3125968118 cites W2035198704 @default.
• W3125968118 cites W2035498751 @default.
• W3125968118 cites W2035919916 @default.
• W3125968118 cites W2039906518 @default.
• W3125968118 cites W2043130320 @default.
• W3125968118 cites W2051533088 @default.
• W3125968118 cites W2058468162 @default.
• W3125968118 cites W2077744352 @default.
• W3125968118 cites W2079648218 @default.
• W3125968118 cites W2080246054 @default.
• W3125968118 cites W2080505426 @default.
• W3125968118 cites W2083217950 @default.
• W3125968118 cites W2088913300 @default.
• W3125968118 cites W2091373511 @default.
• W3125968118 cites W2119285898 @default.
• W3125968118 cites W2120672361 @default.
• W3125968118 cites W2126472162 @default.
• W3125968118 cites W2135125925 @default.
• W3125968118 cites W2137906322 @default.
• W3125968118 cites W2138818566 @default.
• W3125968118 cites W2171003055 @default.
• W3125968118 cites W2224238011 @default.
• W3125968118 cites W2346625407 @default.
• W3125968118 cites W2488308548 @default.
• W3125968118 cites W2952484002 @default.
• W3125968118 cites W2952607039 @default.
• W3125968118 cites W3098640191 @default.
• W3125968118 cites W3099749671 @default.
• W3125968118 cites W3099787294 @default.
• W3125968118 cites W3100150221 @default.
• W3125968118 cites W3101265142 @default.
• W3125968118 cites W3103007029 @default.
• W3125968118 cites W3103347115 @default.
• W3125968118 cites W3104028541 @default.
• W3125968118 cites W3104524431 @default.
• W3125968118 cites W3105434670 @default.
• W3125968118 cites W3105500447 @default.
• W3125968118 cites W3105955606 @default.
• W3125968118 cites W632861426 @default.
• W3125968118 hasPublicationYear "2018" @default.
• W3125968118 type Work @default.
• W3125968118 sameAs 3125968118 @default.
• W3125968118 citedByCount "0" @default.
• W3125968118 crossrefType "journal-article" @default.
• W3125968118 hasAuthorship W3125968118A5031629792 @default.
• W3125968118 hasAuthorship W3125968118A5042881564 @default.
• W3125968118 hasAuthorship W3125968118A5072557695 @default.
• W3125968118 hasAuthorship W3125968118A5073540071 @default.
• W3125968118 hasBestOaLocation W31259681181 @default.
• W3125968118 hasConcept C115260700 @default.
• W3125968118 hasConcept C120665830 @default.
• W3125968118 hasConcept C121332964 @default.
• W3125968118 hasConcept C127592171 @default.
• W3125968118 hasConcept C135757623 @default.
• W3125968118 hasConcept C147789679 @default.
• W3125968118 hasConcept C185592680 @default.
• W3125968118 hasConcept C205049153 @default.
• W3125968118 hasConcept C30475298 @default.
• W3125968118 hasConcept C31532427 @default.
• W3125968118 hasConcept C44870925 @default.
• W3125968118 hasConcept C62520636 @default.
• W3125968118 hasConcept C74902906 @default.
• W3125968118 hasConceptScore W3125968118C115260700 @default.
• W3125968118 hasConceptScore W3125968118C120665830 @default.
• W3125968118 hasConceptScore W3125968118C121332964 @default.
• W3125968118 hasConceptScore W3125968118C127592171 @default.
• W3125968118 hasConceptScore W3125968118C135757623 @default.
• W3125968118 hasConceptScore W3125968118C147789679 @default.
• W3125968118 hasConceptScore W3125968118C185592680 @default.
• W3125968118 hasConceptScore W3125968118C205049153 @default.
• W3125968118 hasConceptScore W3125968118C30475298 @default.
• W3125968118 hasConceptScore W3125968118C31532427 @default.
• W3125968118 hasConceptScore W3125968118C44870925 @default.
• W3125968118 hasConceptScore W3125968118C62520636 @default.

• next