Structure and Evolution of Pre-Main Sequence Stars

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dc.creatorSchulz, Norbert S.
dc.creatorAllen, Glenn
dc.creatorBautz, Mark W.
dc.creatorCanizares, Claude C.
dc.creatorDavis, John
dc.creatorDewey, Dan
dc.creatorHuenemoerder, David P.
dc.creatorHeilmann, Ralf
dc.creatorHouck, John
dc.creatorMarshall, Herman L.
dc.creatorNowak, Mike
dc.creatorSchattenburg, Mark
dc.creatorAudard, Marc
dc.creatorDrake, Jeremy
dc.creatorGagne, Marc
dc.creatorKastner, Joel
dc.creatorKallman, Tim
dc.creatorLautenegger, Maurice
dc.creatorLee, Julia
dc.creatorMiller, Jon
dc.creatorMontmerle, Thierry
dc.creatorMukai, Koji
dc.creatorOsten, Rachel
dc.creatorParerels, Frits
dc.creatorPollock, Andy
dc.creatorPreibisch, Thomas
dc.creatorRaymond, John
dc.creatorReale, Fabio
dc.creatorSmith, Randall
dc.creatorTesta, Paola
dc.creatorWeintraub, David
dc.date2009-04-22
dc.date.accessioned2026-07-07T13:07:13Z
dc.date.available2026-07-07T13:07:13Z
dc.descriptionLow-mass pre-main sequence (PMS) stars are strong and variable X-ray emitters, as has been well established by EINSTEIN and ROSAT observatories. It was originally believed that this emission was of thermal nature and primarily originated from coronal activity (magnetically confined loops, in analogy with Solar activity) on contracting young stars. Broadband spectral analysis showed that the emission was not isothermal and that elemental abundances were non-Solar. The resolving power of the Chandra and XMM X-ray gratings spectrometers have provided the first, tantalizing details concerning the physical conditions such as temperatures, densities, and abundances that characterize the X-ray emitting regions of young star. These existing high resolution spectrometers, however, simply do not have the effective area to measure diagnostic lines for a large number of PMS stars over required to answer global questions such as: how does magnetic activity in PMS stars differ from that of main sequence stars, how do they evolve, what determines the population structure and activity in stellar clusters, and how does the activity influence the evolution of protostellar disks. Highly resolved (R>3000) X-ray spectroscopy at orders of magnitude greater efficiency than currently available will provide major advances in answering these questions. This requires the ability to resolve the key diagnostic emission lines with a precision of better than 100 km/s.
dc.descriptionA White Paper Submitted to the Astro2010 Decadal Survey
dc.identifierhttps://arxiv.org/abs/0904.3385
dc.identifierhttp://arxiv.org/abs/0904.3385
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/228017
dc.subjectHigh Energy Astrophysical Phenomena
dc.subjectAstrophysics of Galaxies
dc.titleStructure and Evolution of Pre-Main Sequence Stars
dc.typetext

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