FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W1997254846> ?p ?o ?g. }

• W1997254846 endingPage "1161" @default.
• W1997254846 startingPage "1145" @default.
• W1997254846 abstract "The origin of magnetic fields in intermediate- and high-mass stars is fundamentally a mystery. Clues towards solving this basic astrophysical problem can likely be found at the pre-main-sequence (PMS) evolutionary stage. With this work, we perform the largest and most sensitive search for magnetic fields in PMS Herbig Ae/Be (HAeBe) stars. We seek to determine whether strong, ordered magnetic fields, similar to those of main-sequence Ap/Bp stars, can be detected in these objects, and if so, to determine the intensities, geometrical characteristics, and statistical incidence of such fields. 68 observations of 50 HAeBe stars have been obtained in circularly polarized light using the FORS 1 spectropolarimeter at the ESO VLT. An analysis of both Balmer and metallic lines reveals the possible presence of weak longitudinal magnetic fields in photospheric lines of two HAeBe stars, HD 101412 and BF Ori. Results for two additional stars, CPD-53 295 and HD 36112, are suggestive of the presence of magnetic fields, but no firm conclusions can be drawn based on the available data. The intensity of the longitudinal fields detected in HD 101412 and BF Ori suggest that they correspond to globally ordered magnetic fields with surface intensities of order 1 kG. On the other hand, no magnetic field is detected in 4 other HAeBe stars in our sample in which magnetic fields had previously been confirmed. Monte Carlo simulations of the longitudinal field measurements of the undetected stars allow us to place an upper limit of about 300 G on the general presence of aligned magnetic dipole magnetic fields, and of about 500 G on perpendicular dipole fields. Taking into account the results of our survey and other published results, we find that the observed bulk incidence of magnetic HAeBe stars in our sample is 8-12 per cent, in good agreement with that of magnetic main-sequence stars of similar masses. We also find that the rms longitudinal field intensity of magnetically detected HAeBe stars is about 200 G, similar to that of Ap stars and consistent with magnetic flux conservation during stellar evolution. These results are all in agreement with the hypothesis that the magnetic fields of main-sequence Ap/Bp stars are fossils, which already exist within the stars at the PMS stage. Finally, we explore the ability of our new magnetic data to constrain magnetospheric accretion in Herbig Ae/Be stars, showing that our magnetic data are not consistent with the general occurrence in HAeBe stars of magnetospheric accretion as described by the theories of Konigl and Shu et al.." @default.
• W1997254846 created "2016-06-24" @default.
• W1997254846 creator A5014887556 @default.
• W1997254846 creator A5031474913 @default.
• W1997254846 creator A5050609121 @default.
• W1997254846 creator A5072935646 @default.
• W1997254846 creator A5087141427 @default.
• W1997254846 date "2007-04-11" @default.
• W1997254846 modified "2023-09-30" @default.
• W1997254846 title "A search for strong, ordered magnetic fields in Herbig Ae/Be stars" @default.
• W1997254846 cites W182415305 @default.
• W1997254846 cites W1970608130 @default.
• W1997254846 cites W1974761233 @default.
• W1997254846 cites W1978391636 @default.
• W1997254846 cites W1978682732 @default.
• W1997254846 cites W1979218713 @default.
• W1997254846 cites W1981884171 @default.
• W1997254846 cites W1998015699 @default.
• W1997254846 cites W2002290949 @default.
• W1997254846 cites W2006827586 @default.
• W1997254846 cites W2010997879 @default.
• W1997254846 cites W2014836068 @default.
• W1997254846 cites W2017311127 @default.
• W1997254846 cites W2021272563 @default.
• W1997254846 cites W2023344645 @default.
• W1997254846 cites W2030798973 @default.
• W1997254846 cites W2044419757 @default.
• W1997254846 cites W2052248972 @default.
• W1997254846 cites W2053648858 @default.
• W1997254846 cites W2065378328 @default.
• W1997254846 cites W2068843564 @default.
• W1997254846 cites W2076860618 @default.
• W1997254846 cites W2080329963 @default.
• W1997254846 cites W2085095213 @default.
• W1997254846 cites W2086180078 @default.
• W1997254846 cites W2087448967 @default.
• W1997254846 cites W2097412590 @default.
• W1997254846 cites W2097706132 @default.
• W1997254846 cites W2098149182 @default.
• W1997254846 cites W2100812183 @default.
• W1997254846 cites W2101422080 @default.
• W1997254846 cites W2101651466 @default.
• W1997254846 cites W2107028611 @default.
• W1997254846 cites W2123144427 @default.
• W1997254846 cites W2123210711 @default.
• W1997254846 cites W2125314121 @default.
• W1997254846 cites W2125486253 @default.
• W1997254846 cites W2125500606 @default.
• W1997254846 cites W2127867276 @default.
• W1997254846 cites W2129099507 @default.
• W1997254846 cites W2142050845 @default.
• W1997254846 cites W2142722860 @default.
• W1997254846 cites W2152528559 @default.
• W1997254846 cites W2158174512 @default.
• W1997254846 cites W2161973129 @default.
• W1997254846 cites W2162411080 @default.
• W1997254846 cites W2164167034 @default.
• W1997254846 cites W2167268859 @default.
• W1997254846 cites W3101646687 @default.
• W1997254846 cites W4289813091 @default.
• W1997254846 doi "https://doi.org/10.1111/j.1365-2966.2007.11495.x" @default.
• W1997254846 hasPublicationYear "2007" @default.
• W1997254846 type Work @default.
• W1997254846 sameAs 1997254846 @default.
• W1997254846 citedByCount "120" @default.
• W1997254846 countsByYear W19972548462012 @default.
• W1997254846 countsByYear W19972548462013 @default.
• W1997254846 countsByYear W19972548462014 @default.
• W1997254846 countsByYear W19972548462015 @default.
• W1997254846 countsByYear W19972548462016 @default.
• W1997254846 countsByYear W19972548462017 @default.
• W1997254846 countsByYear W19972548462018 @default.
• W1997254846 countsByYear W19972548462019 @default.
• W1997254846 countsByYear W19972548462020 @default.
• W1997254846 countsByYear W19972548462021 @default.
• W1997254846 countsByYear W19972548462022 @default.
• W1997254846 countsByYear W19972548462023 @default.
• W1997254846 crossrefType "journal-article" @default.
• W1997254846 hasAuthorship W1997254846A5014887556 @default.
• W1997254846 hasAuthorship W1997254846A5031474913 @default.
• W1997254846 hasAuthorship W1997254846A5050609121 @default.
• W1997254846 hasAuthorship W1997254846A5072935646 @default.
• W1997254846 hasAuthorship W1997254846A5087141427 @default.
• W1997254846 hasBestOaLocation W19972548462 @default.
• W1997254846 hasConcept C115260700 @default.
• W1997254846 hasConcept C121332964 @default.
• W1997254846 hasConcept C1276947 @default.
• W1997254846 hasConcept C1329718 @default.
• W1997254846 hasConcept C150846664 @default.
• W1997254846 hasConcept C178075534 @default.
• W1997254846 hasConcept C44870925 @default.
• W1997254846 hasConcept C62520636 @default.
• W1997254846 hasConcept C80518518 @default.
• W1997254846 hasConceptScore W1997254846C115260700 @default.
• W1997254846 hasConceptScore W1997254846C121332964 @default.
• W1997254846 hasConceptScore W1997254846C1276947 @default.
• W1997254846 hasConceptScore W1997254846C1329718 @default.
• W1997254846 hasConceptScore W1997254846C150846664 @default.

• next