SwePub
Sök i LIBRIS databas

  Utökad sökning

id:"swepub:oai:research.chalmers.se:fd94a532-90a8-4713-9a8b-ad0ef67e5ee1"
 

Sökning: id:"swepub:oai:research.chalmers.se:fd94a532-90a8-4713-9a8b-ad0ef67e5ee1" > Search for high-mas...

LIBRIS Formathandbok  (Information om MARC21)
FältnamnIndikatorerMetadata
00007500naa a2200637 4500
001oai:research.chalmers.se:fd94a532-90a8-4713-9a8b-ad0ef67e5ee1
003SwePub
008181015s2018 | |||||||||||000 ||eng|
0247 a https://research.chalmers.se/publication/5055542 URI
0247 a https://doi.org/10.1051/0004-6361/2018327532 DOI
0247 a https://research.chalmers.se/publication/5063272 URI
0247 a https://research.chalmers.se/publication/5054012 URI
0247 a https://research.chalmers.se/publication/5053762 URI
040 a (SwePub)cth
041 a engb eng
042 9 SwePub
072 7a art2 swepub-publicationtype
072 7a ref2 swepub-contenttype
1001 a Csengeri, T.u Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)4 aut
2451 0a Search for high-mass protostars with ALMA revealed up to kilo-parsec scales (SPARKS): I. Indication for a centrifugal barrier in the environment of a single high-mass envelope
264 c 2018-09-21
264 1b EDP Sciences,c 2018
338 a electronic2 rdacarrier
520 a The conditions leading to the formation of the most massive O-type stars are still an enigma in modern astrophysics. To assess the physical conditions of high-mass protostars in their main accretion phase, here we present a case study of a young massive clump selected from the ATLASGAL survey, G328.2551-0.5321. The source exhibits a bolometric luminosity of 1.3 × 104L·, which allows us to estimate that its current protostellar mass lies between ∼11 and 16 M·. We show high angular resolution observations with ALMA that reach a physical scale of ∼400 au. To reveal the structure of this high-mass protostellar envelope in detail at a ∼0.17′′ resolution, we used the thermal dust continuum emission and spectroscopic information, amongst others from the CO (J = 3-2) line, which is sensitive to the high-velocity molecular outflow of the source. We also used the SiO (J = 8-7) and SO2(J = 82,6-71,7) lines, which trace shocks along the outflow, as well as several CH3OH and HC3N lines that probe the gas of the inner envelope in the closest vicinity of the protostar. Our observations of the dust continuum emission reveal a single high-mass protostellar envelope, down to our resolution limit. We find evidence for a compact, marginally resolved continuum source that is surrounded by azimuthal elongations that could be consistent with a spiral pattern. We also report on the detection of a rotational line of CH3OH within its vt= 1 torsionally excited state. This shows two bright emission peaks that are spatially offset from the dust continuum peak and exhibit a distinct velocity component ±4.5 km s-1offset from the systemic velocity of the source. Rotational diagram analysis and models based on local thermodynamic equilibrium assumption require high CH3OH column densities that reach N(CH3OH) = 1.2-2 × 1019cm-2, and kinetic temperatures of the order of 160-200 K at the position of these peaks. A comparison of their morphology and kinematics with those of the outflow component of the CO line and the SO2line suggests that the high-excitation CH3OH spots are associated with the innermost regions of the envelope. While the HC3N v7= 0 (J = 37-36) line is also detected in the outflow, the HC3N v7= 1e (J = 38-37) rotational transition within the first vibrationally excited state of the molecule shows a compact morphology. We find that the velocity shifts at the position of the observed high-excitation CH3OH spots correspond well to the expected Keplerian velocity around a central object with 15 M·consistent with the mass estimate based on the bolometric luminosity of the source. We propose a picture where the CH3OH emission peaks trace the accretion shocks around the centrifugal barrier, pinpointing the interaction region between the collapsing envelope and an accretion disc. The physical properties of the accretion disc inferred from these observations suggest a specific angular momentum several times higher than typically observed towards low-mass protostars. This is consistent with a scenario of global collapse setting on at larger scales that could carry a more significant amount of kinetic energy compared to the core-collapse models of low-mass star formation. Furthermore, our results suggest that vibrationally excited HC3N emission could be a new tracer for compact accretion discs around high-mass protostars.
650 7a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng
650 7a NATURVETENSKAPx Fysikx Atom- och molekylfysik och optik0 (SwePub)103022 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Atom and Molecular Physics and Optics0 (SwePub)103022 hsv//eng
650 7a NATURVETENSKAPx Fysikx Annan fysik0 (SwePub)103992 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Other Physics Topics0 (SwePub)103992 hsv//eng
653 a Stars: massive
653 a Stars: formation
653 a Submillimeter: ISM
653 a Accretion, accretion disks
7001 a Bontemps, S.u Observatoire Aquitain des Sciences de l'Univers, OASU4 aut
7001 a Wyrowski, F.u Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)4 aut
7001 a Belloche, A.u Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)4 aut
7001 a Menten, K.u Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)4 aut
7001 a Leurini, S.u Istituto nazionale di astrofisica (INAF)4 aut
7001 a Beuther, H.u Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)4 aut
7001 a Bronfman, Leonardou Universidad de Chile (UCH),University of Chile (UCH)4 aut
7001 a Commerçon, B.u École Normale Supérieure de Lyon4 aut
7001 a Chapillon, E.u Institut de Radioastronomie Millimétrique (IRAM),Observatoire Aquitain des Sciences de l'Univers, OASU4 aut
7001 a Longmore, S.u Liverpool John Moores University4 aut
7001 a Palau, A.u Universidad Nacional Autónoma de México (UNAM),Universidad Nacional Autonoma de Mexico4 aut
7001 a Tan, Jonathan,d 1973u University of Virginia,Chalmers tekniska högskola,Chalmers University of Technology4 aut0 (Swepub:cth)tanj
7001 a Urquhart, J. S.u University Of Kent4 aut
7102 a Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG)b Observatoire Aquitain des Sciences de l'Univers, OASU4 org
7730 t Astronomy and Astrophysicsd : EDP Sciencesg 617q 617x 0004-6361x 1432-0746
8564 u https://research.chalmers.se/publication/506327/file/506327_Fulltext.pdfx primaryx freey FULLTEXT
8564 u https://www.aanda.org/articles/aa/pdf/2018/09/aa32753-18.pdf
8564 8u https://research.chalmers.se/publication/505554
8564 8u https://doi.org/10.1051/0004-6361/201832753
8564 8u https://research.chalmers.se/publication/506327
8564 8u https://research.chalmers.se/publication/505401
8564 8u https://research.chalmers.se/publication/505376

Hitta via bibliotek

Till lärosätets databas

Kungliga biblioteket hanterar dina personuppgifter i enlighet med EU:s dataskyddsförordning (2018), GDPR. Läs mer om hur det funkar här.
Så här hanterar KB dina uppgifter vid användning av denna tjänst.

 
pil uppåt Stäng

Kopiera och spara länken för att återkomma till aktuell vy