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LIBRIS Formathandbok  (Information om MARC21)
FältnamnIndikatorerMetadata
00008251naa a2200865 4500
001oai:research.chalmers.se:5c5b2843-069b-4fcb-8bfc-caac5bd33a2d
003SwePub
008191114s2019 | |||||||||||000 ||eng|
009oai:lup.lub.lu.se:79572d6c-cba3-4f03-a397-276a2866d808
0247 a https://doi.org/10.1051/0004-6361/2019353402 DOI
0247 a https://research.chalmers.se/publication/5137512 URI
0247 a https://lup.lub.lu.se/record/79572d6c-cba3-4f03-a397-276a2866d8082 URI
040 a (SwePub)cthd (SwePub)lu
041 a engb eng
042 9 SwePub
072 7a art2 swepub-publicationtype
072 7a ref2 swepub-contenttype
1001 a Coutens, A.u Université de Bordeaux,University of Bordeaux4 aut
2451 0a VLA cm-wave survey of young stellar objects in the Oph A cluster: Constraining extreme UV- And X-ray-driven disk photoevaporation: A pathfinder for Square Kilometre Array studies
264 c 2019-10-21
264 1b EDP Sciences,c 2019
338 a electronic2 rdacarrier
520 a Observations of young stellar objects (YSOs) in centimeter bands can probe the continuum emission from growing dust grains, ionized winds, and magnetospheric activity that are intimately connected to the evolution of protoplanetary disks and the formation of planets. We carried out sensitive continuum observations toward the Ophiuchus A star-forming region, using the Karl G. Jansky Very Large Array (VLA) at 10 GHz over a field-of-view of 6′ and with a spatial resolution of θmaj ×θmin ∼ 0.′′4 × 0.′′2. We achieved a 5 μJy beam-1 rms noise level at the center of our mosaic field of view. Among the 18 sources we detected, 16 were YSOs (three Class 0, five Class I, six Class II, and two Class III) and two were extragalactic candidates. We find that thermal dust emission generally contributed less than 30% of the emission at 10 GHz. The radio emission is dominated by other types of emission, such as gyro-synchrotron radiation from active magnetospheres, free-free emission from thermal jets, free-free emission from the outflowing photoevaporated disk material, and synchrotron emission from accelerated cosmic-rays in jet or protostellar surface shocks. These different types of emission could not be clearly disentangled. Our non-detections for Class II/III disks suggest that extreme UV-driven photoevaporation is insufficient to explain disk dispersal, assuming that the contribution of UV photoevaporating stellar winds to radio flux does not evolve over time. The sensitivity of our data cannot exclude photoevaporation due to the role of X-ray photons as an efficient mechanism for disk dispersal. Deeper surveys using the Square Kilometre Array (SKA) will have the capacity to provide significant constraints to disk photoevaporation.
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 Fusion, plasma och rymdfysik0 (SwePub)103032 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Fusion, Plasma and Space Physics0 (SwePub)103032 hsv//eng
653 a Stars: formation
653 a Protoplanetary disks
653 a Radio continuum: stars
653 a Stars: activity
653 a Protoplanetary disks
653 a Radio continuum: stars
653 a Stars: activity
653 a Stars: formation
7001 a Liu, H. B.u European Southern Observatory (ESO),European Southern Observatory4 aut
7001 a Jimenez-Serra, I.u Queen Mary University of London,Queen Mary University4 aut
7001 a Bourke, T. L.u SKA Organisation,SKA Organisation, UK,National Autonomous University of Mexico,INAF - Osservatorio Astrofisico di Arcetri,European Southern Observatory4 aut
7001 a Forbrich, J.u University of Hertfordshire4 aut
7001 a Hoare, M. G.u University of Leeds4 aut
7001 a Loinard, L.u Universidad Nacional Autónoma de México (UNAM),Universidad Nacional Autonoma de Mexico,University of Chile,INAF - Osservatorio Astrofisico di Arcetri4 aut
7001 a Testi, L.u Osservatorio Astrofisico di Arcetri,Arcetri Astrophysical Observatory,European Southern Observatory (ESO)4 aut
7001 a Audard, M.u Université de Genève,University of Geneva4 aut
7001 a Caselli, P.u Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG),Max Planck Institute for Extraterrestrial Physics4 aut
7001 a Chacón-Tanarro, A.u Observatorio Astronómico Nacional (OAN),Spanish National Observatory (OAN),Observatorio Astronómico Nacional (OAG-IGN)4 aut
7001 a Codella, C.u Université Grenoble Alpes,Grenoble Alpes University,Osservatorio Astrofisico di Arcetri,Arcetri Astrophysical Observatory,INAF - Osservatorio Astrofisico di Arcetri,University Grenoble Alpes,University College London,University of Leeds4 aut
7001 a Di Francesco, J.u National Research Council Canada,University of Victoria,NRC Herzberg Institute of Astrophysics (NRC-HIA)4 aut
7001 a Fontani, Francescou Osservatorio Astrofisico di Arcetri,Arcetri Astrophysical Observatory,INAF - Osservatorio Astrofisico di Arcetri4 aut
7001 a Hogerheijde, M.u Universiteit Leiden (UL),Leiden University (UL),Universiteit Van Amsterdam,University of Amsterdam,Leiden University,Netherlands Institute for Radio Astronomy (ASTRON)4 aut
7001 a Johansen, A.u Lund University,Lunds universitet,Astronomi - Genomgår omorganisation,Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation,Naturvetenskapliga fakulteten,Lund Observatory - Undergoing reorganization,Department of Astronomy and Theoretical Physics - Undergoing reorganization,Faculty of Science4 aut0 (Swepub:lu)astr-arj
7001 a Johnstone, D.u National Research Council Canada,University of Victoria4 aut
7001 a Maddison, S.u Swinburne University of Technology4 aut
7001 a Panić, O.u University of Leeds4 aut
7001 a Perez, L.u Universidad de Chile (UCH),University of Chile (UCH)4 aut
7001 a Podio, L.u Osservatorio Astrofisico di Arcetri,Arcetri Astrophysical Observatory4 aut
7001 a Punanova, A.u Ural Federal University4 aut
7001 a Rawlings, J. M.C.u University College London (UCL)4 aut
7001 a Semenov, D.u Ludwig-Maximilians-Universität München,Ludwig Maximilian University of Munich,Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG),Max Planck Institute for Astronomy,Ludwig-Maximilian University of Munich4 aut
7001 a Tazzari, M.u University Of Cambridge,University of Cambridge4 aut
7001 a Tobin, J. J.u National Radio Astronomy Observatory4 aut
7001 a van der Wiel, M. H. D.u Netherlands Institute for Radio Astronomy (ASTRON)4 aut
7001 a van Langevelde, H. J.u Joint Institute for VLBI in Europe (JIVE),University of Victoria4 aut
7001 a Vlemmings, Wouter,d 1974u Chalmers University of Technology4 aut0 (Swepub:cth)wouterv
7001 a Walsh, C.u University of Leeds4 aut
7001 a Wilner, D. J.u Harvard-Smithsonian Center for Astrophysics,Harvard–Smithsonian Center for Astrophysics4 aut
7102 a Université de Bordeauxb University of Bordeaux4 org
7730 t Astronomy and Astrophysicsd : EDP Sciencesg 631q 631x 0004-6361x 1432-0746
8564 u https://research.chalmers.se/publication/513751/file/513751_Fulltext.pdfx primaryx freey FULLTEXT
8564 u https://www.aanda.org/articles/aa/pdf/2019/11/aa35340-19.pdf
8564 u http://dx.doi.org/10.1051/0004-6361/201935340x freey FULLTEXT
8564 8u https://doi.org/10.1051/0004-6361/201935340
8564 8u https://research.chalmers.se/publication/513751
8564 8u https://lup.lub.lu.se/record/79572d6c-cba3-4f03-a397-276a2866d808

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