FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W2010367631> ?p ?o ?g. }

• W2010367631 endingPage "300" @default.
• W2010367631 startingPage "278" @default.
• W2010367631 abstract "Determining temperatures in molecular clouds from ratios of CO rotational lines or from ratios of continuum emission in different wavelength bands suffers from reduced temperature sensitivity in the high-temperature limit. In theory, the ratio of far-infrared (FIR), submillimetre or millimetre continuum to that of a 13 CO (or C 18 O) rotational line can place reliable upper limits on the temperature of the dust and molecular gas. Consequently, FIR continuum data from the COBE/Diffuse Infrared Background Experiment (DIRBE) instrument and Nagoya 4-m 13 COJ = 1 → 0 spectral line data were used to plot 240 μm/ 13 COJ = 1 → 0 intensity ratios against 140/240 μm dust colour temperatures, allowing us to constrain the multiparsec-scale physical conditions in the Orion A and B molecular clouds. The best-fitting models to the Orion clouds consist of two components: a component near the surface of the clouds that is heated primarily by a very large scale (i.e. ∼1 kpc) interstellar radiation field and a component deeper within the clouds. The former has a fixed temperature and the latter has a range of temperatures that vary from one sightline to another. The models require a dust-gas temperature difference of 0 ± 2 K and suggest that 40-50 per cent of the Orion clouds are in the form of dust and gas with temperatures between 3 and 10K. The implications are discussed in detail in later papers and include stronger dust-gas thermal coupling and higher Galactic-scale molecular gas temperatures than are usually accepted, and an improved explanation for the N(H 2 )/I(CO) conversion factor. It is emphasized that these results are preliminary and require confirmation by independent observations and methods." @default.
• W2010367631 created "2016-06-24" @default.
• W2010367631 creator A5076411236 @default.
• W2010367631 date "2007-02-11" @default.
• W2010367631 modified "2023-09-23" @default.
• W2010367631 title "Comparison of 13CO line and far-infrared continuum emission as a diagnostic of dust and molecular gas physical conditions - I. Motivation and modelling" @default.
• W2010367631 cites W1504479788 @default.
• W2010367631 cites W1540491343 @default.
• W2010367631 cites W1605144396 @default.
• W2010367631 cites W1626033413 @default.
• W2010367631 cites W1645561024 @default.
• W2010367631 cites W1965359410 @default.
• W2010367631 cites W1970735236 @default.
• W2010367631 cites W1973003901 @default.
• W2010367631 cites W1973063375 @default.
• W2010367631 cites W1973086534 @default.
• W2010367631 cites W1974563018 @default.
• W2010367631 cites W1974611967 @default.
• W2010367631 cites W1975789754 @default.
• W2010367631 cites W1976666257 @default.
• W2010367631 cites W1976715677 @default.
• W2010367631 cites W1978975187 @default.
• W2010367631 cites W1983659778 @default.
• W2010367631 cites W1985666257 @default.
• W2010367631 cites W1991854655 @default.
• W2010367631 cites W1994568579 @default.
• W2010367631 cites W1995435934 @default.
• W2010367631 cites W1996425412 @default.
• W2010367631 cites W1997632510 @default.
• W2010367631 cites W1997972076 @default.
• W2010367631 cites W1998762398 @default.
• W2010367631 cites W1999046469 @default.
• W2010367631 cites W1999313864 @default.
• W2010367631 cites W2001274357 @default.
• W2010367631 cites W2001551929 @default.
• W2010367631 cites W2004991911 @default.
• W2010367631 cites W2006730595 @default.
• W2010367631 cites W2009145211 @default.
• W2010367631 cites W2009759483 @default.
• W2010367631 cites W2011685385 @default.
• W2010367631 cites W2014059545 @default.
• W2010367631 cites W2016384036 @default.
• W2010367631 cites W2018936248 @default.
• W2010367631 cites W2023409203 @default.
• W2010367631 cites W2028739552 @default.
• W2010367631 cites W2031916992 @default.
• W2010367631 cites W2033012896 @default.
• W2010367631 cites W2035152140 @default.
• W2010367631 cites W2037239973 @default.
• W2010367631 cites W2038219046 @default.
• W2010367631 cites W2038851261 @default.
• W2010367631 cites W2043638572 @default.
• W2010367631 cites W2046681938 @default.
• W2010367631 cites W2055506692 @default.
• W2010367631 cites W2059309055 @default.
• W2010367631 cites W2063000920 @default.
• W2010367631 cites W2063480023 @default.
• W2010367631 cites W2064528785 @default.
• W2010367631 cites W2064666376 @default.
• W2010367631 cites W2073218926 @default.
• W2010367631 cites W2074566797 @default.
• W2010367631 cites W2077287923 @default.
• W2010367631 cites W2078001023 @default.
• W2010367631 cites W2078102957 @default.
• W2010367631 cites W2078658496 @default.
• W2010367631 cites W2086140797 @default.
• W2010367631 cites W2089469010 @default.
• W2010367631 cites W2089535760 @default.
• W2010367631 cites W2090062386 @default.
• W2010367631 cites W2090923496 @default.
• W2010367631 cites W2094423975 @default.
• W2010367631 cites W2107308018 @default.
• W2010367631 cites W2133198903 @default.
• W2010367631 cites W2142255666 @default.
• W2010367631 cites W2951335256 @default.
• W2010367631 cites W3098104912 @default.
• W2010367631 cites W3099112362 @default.
• W2010367631 cites W3099590149 @default.
• W2010367631 cites W3099830973 @default.
• W2010367631 cites W3100298884 @default.
• W2010367631 cites W3100429490 @default.
• W2010367631 cites W3102898013 @default.
• W2010367631 cites W3123551154 @default.
• W2010367631 cites W3167005496 @default.
• W2010367631 cites W3174308525 @default.
• W2010367631 cites W4237048634 @default.
• W2010367631 cites W4255119503 @default.
• W2010367631 doi "https://doi.org/10.1111/j.1365-2966.2006.11293.x" @default.
• W2010367631 hasPublicationYear "2007" @default.
• W2010367631 type Work @default.
• W2010367631 sameAs 2010367631 @default.
• W2010367631 citedByCount "4" @default.
• W2010367631 countsByYear W20103676312012 @default.
• W2010367631 crossrefType "journal-article" @default.
• W2010367631 hasAuthorship W2010367631A5076411236 @default.
• W2010367631 hasBestOaLocation W20103676312 @default.
• W2010367631 hasConcept C121332964 @default.
• W2010367631 hasConcept C1276947 @default.

• next