FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W2041195641> ?p ?o ?g. }

• W2041195641 endingPage "118" @default.
• W2041195641 startingPage "104" @default.
• W2041195641 abstract "Echelle spectroscopy of H22.122μm, [Feii]1.644μm and Brγ line emission from a very young planetary nebula (PN), IRAS21282+5050, and from four protoplanetary nebulae (PPN), IRAS 19343+2926 (M1−92), IRAS17150−3224 (AFGL 6815), IRAS17423−1755 (Hen 3−1475) and IRAS17441−2411, is presented. H2 line emission is detected in discrete shock fronts in the lobes of each nebula, regardless of source spectral type [although non-detections in IRAS 09371+1212 (Frosty Leo) support claims that late spectral types do not produce bright H2 line emission]. In IRAS17150−3224, we also uncover possible signs of rotation, as would be expected if the H2 features were excited in a magnetocentrifugal disc wind. [Feii]1.644μm emission was detected in only one source, M1−92 (notably, the source with the brightest H2 features). Again, the emission is predominantly excited in high-velocity shocks in the bipolar lobes of the PPN. The H2 and [Feii] observations of M1−92, and the complex H2 profiles in IRAS21282+5050, are explained using the shock models of Smith and collaborators. We show that bow shock models are generally able to account for the observed line profiles, peak velocities, the double-peaked profiles in IRAS21282+5050, and the spatial distribution of H2 and [Feii] in M 1−92. J-type bow models are adequate in each case, i.e. a strongly magnetized wind is not required. Finally, Brγ is detected in each of the five targets; in absorption in the G-type PPN, though in emission in the O- and B-type sources. Brγ emission is detected predominantly towards the near-infrared (near-IR) continuum peak in each PPN, with only very weak emission detected in the extended lobes of the O- and B-type sources. In Brγ, low peak velocities, though very broad profile widths, are measured in each target, regardless of the nebula inclination angle. The emission must therefore derive from ionized regions in a fast wind very close to the central star (rather than from shocks in the bipolar lobes), or, in the late-type sources, from absorption in an equatorial torus." @default.
• W2041195641 created "2016-06-24" @default.
• W2041195641 creator A5017439674 @default.
• W2041195641 creator A5040950031 @default.
• W2041195641 creator A5049451260 @default.
• W2041195641 creator A5080226981 @default.
• W2041195641 date "2005-06-01" @default.
• W2041195641 modified "2023-09-26" @default.
• W2041195641 title "Near-infrared echelle spectroscopy of protoplanetary nebulae: probing the fast wind in H₂" @default.
• W2041195641 cites W1624677845 @default.
• W2041195641 cites W1633563739 @default.
• W2041195641 cites W1679063286 @default.
• W2041195641 cites W1966195437 @default.
• W2041195641 cites W1966821842 @default.
• W2041195641 cites W1970113028 @default.
• W2041195641 cites W1975403813 @default.
• W2041195641 cites W1986018258 @default.
• W2041195641 cites W1987753284 @default.
• W2041195641 cites W1988544821 @default.
• W2041195641 cites W1991328280 @default.
• W2041195641 cites W1998377814 @default.
• W2041195641 cites W2004636863 @default.
• W2041195641 cites W2007156045 @default.
• W2041195641 cites W2017891779 @default.
• W2041195641 cites W2018932319 @default.
• W2041195641 cites W2019781988 @default.
• W2041195641 cites W2030490016 @default.
• W2041195641 cites W2033579274 @default.
• W2041195641 cites W2040980429 @default.
• W2041195641 cites W2041127269 @default.
• W2041195641 cites W2052876174 @default.
• W2041195641 cites W2053520527 @default.
• W2041195641 cites W2054040364 @default.
• W2041195641 cites W2054837259 @default.
• W2041195641 cites W2056979425 @default.
• W2041195641 cites W2058467858 @default.
• W2041195641 cites W2060576169 @default.
• W2041195641 cites W2060966154 @default.
• W2041195641 cites W2064302459 @default.
• W2041195641 cites W2072437672 @default.
• W2041195641 cites W2072715697 @default.
• W2041195641 cites W2075365172 @default.
• W2041195641 cites W2079112460 @default.
• W2041195641 cites W2081087406 @default.
• W2041195641 cites W2086726391 @default.
• W2041195641 cites W2100222195 @default.
• W2041195641 cites W2105675702 @default.
• W2041195641 cites W2115008877 @default.
• W2041195641 cites W2115811656 @default.
• W2041195641 cites W2116627635 @default.
• W2041195641 cites W2123559115 @default.
• W2041195641 cites W2130176353 @default.
• W2041195641 cites W2142962633 @default.
• W2041195641 cites W2153692635 @default.
• W2041195641 cites W2166956210 @default.
• W2041195641 cites W3044489730 @default.
• W2041195641 cites W3099510838 @default.
• W2041195641 cites W3100012892 @default.
• W2041195641 cites W3100971321 @default.
• W2041195641 cites W3106237422 @default.
• W2041195641 cites W4300187264 @default.
• W2041195641 cites W85711916 @default.
• W2041195641 doi "https://doi.org/10.1111/j.1365-2966.2005.09018.x" @default.
• W2041195641 hasPublicationYear "2005" @default.
• W2041195641 type Work @default.
• W2041195641 sameAs 2041195641 @default.
• W2041195641 citedByCount "19" @default.
• W2041195641 countsByYear W20411956412014 @default.
• W2041195641 countsByYear W20411956412016 @default.
• W2041195641 countsByYear W20411956412019 @default.
• W2041195641 countsByYear W20411956412020 @default.
• W2041195641 countsByYear W20411956412022 @default.
• W2041195641 countsByYear W20411956412023 @default.
• W2041195641 crossrefType "journal-article" @default.
• W2041195641 hasAuthorship W2041195641A5017439674 @default.
• W2041195641 hasAuthorship W2041195641A5040950031 @default.
• W2041195641 hasAuthorship W2041195641A5049451260 @default.
• W2041195641 hasAuthorship W2041195641A5080226981 @default.
• W2041195641 hasBestOaLocation W20411956412 @default.
• W2041195641 hasConcept C121332964 @default.
• W2041195641 hasConcept C1276947 @default.
• W2041195641 hasConcept C150846664 @default.
• W2041195641 hasConcept C155991500 @default.
• W2041195641 hasConcept C181500209 @default.
• W2041195641 hasConcept C184779094 @default.
• W2041195641 hasConcept C198352243 @default.
• W2041195641 hasConcept C2524010 @default.
• W2041195641 hasConcept C2779496878 @default.
• W2041195641 hasConcept C32891209 @default.
• W2041195641 hasConcept C33923547 @default.
• W2041195641 hasConcept C44870925 @default.
• W2041195641 hasConcept C4839761 @default.
• W2041195641 hasConcept C70477161 @default.
• W2041195641 hasConcept C95373548 @default.
• W2041195641 hasConcept C96141758 @default.
• W2041195641 hasConcept C97355855 @default.
• W2041195641 hasConceptScore W2041195641C121332964 @default.
• W2041195641 hasConceptScore W2041195641C1276947 @default.

• next