Structure and Evolution of Pre-Main Sequence Stars

Low-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...

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Main Authors: Schulz, Norbert S., Allen, Glenn E., Bautz, Mark W., Canizares, Claude R., Davis, John E., Dewey, Dan, Huenemoerder, David P., Heilmann, Ralf K., Houck, John C., Marshall, Herman Lee, Nowak, Michael A., Schattenburg, Mark
Other Authors: MIT Kavli Institute for Astrophysics and Space Research
Format: Article
Language:en_US
Published: National Academy of Sciences 2013
Online Access:http://hdl.handle.net/1721.1/77613
https://orcid.org/0000-0001-6932-2612
https://orcid.org/0000-0002-1379-4482
https://orcid.org/0000-0002-5769-8441
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author Schulz, Norbert S.
Allen, Glenn E.
Bautz, Mark W.
Canizares, Claude R.
Davis, John E.
Dewey, Dan
Huenemoerder, David P.
Heilmann, Ralf K.
Houck, John C.
Marshall, Herman Lee
Nowak, Michael A.
Schattenburg, Mark
author2 MIT Kavli Institute for Astrophysics and Space Research
author_facet MIT Kavli Institute for Astrophysics and Space Research
Schulz, Norbert S.
Allen, Glenn E.
Bautz, Mark W.
Canizares, Claude R.
Davis, John E.
Dewey, Dan
Huenemoerder, David P.
Heilmann, Ralf K.
Houck, John C.
Marshall, Herman Lee
Nowak, Michael A.
Schattenburg, Mark
author_sort Schulz, Norbert S.
collection MIT
description Low-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.
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spelling mit-1721.1/776132022-10-01T09:52:16Z Structure and Evolution of Pre-Main Sequence Stars Schulz, Norbert S. Allen, Glenn E. Bautz, Mark W. Canizares, Claude R. Davis, John E. Dewey, Dan Huenemoerder, David P. Heilmann, Ralf K. Houck, John C. Marshall, Herman Lee Nowak, Michael A. Schattenburg, Mark MIT Kavli Institute for Astrophysics and Space Research Schulz, Norbert S. Allen, Glenn E. Bautz, Mark W. Canizares, Claude R. Davis, John E. Dewey, Dan Huenemoerder, David P. Heilmann, Ralf K. Houck, John C. Marshall, Herman Lee Nowak, Michael A. Schattenburg, Mark Low-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. 2013-03-11T15:04:24Z 2013-03-11T15:04:24Z 2009 2009-04 Article http://purl.org/eprint/type/JournalArticle http://hdl.handle.net/1721.1/77613 Glenn Allen et al. "Structure and Evolution of Pre-Main Sequence." Astro2010: The Astronomy and Astrophysics Decadal Survey, National Academies 2010. https://orcid.org/0000-0001-6932-2612 https://orcid.org/0000-0002-1379-4482 https://orcid.org/0000-0002-5769-8441 en_US http://www8.nationalacademies.org/astro2010/DetailFileDisplay.aspx?id=40 Astro2010: The Astronomy and Astrophysics Decadal Survey Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. application/pdf National Academy of Sciences arVix
spellingShingle Schulz, Norbert S.
Allen, Glenn E.
Bautz, Mark W.
Canizares, Claude R.
Davis, John E.
Dewey, Dan
Huenemoerder, David P.
Heilmann, Ralf K.
Houck, John C.
Marshall, Herman Lee
Nowak, Michael A.
Schattenburg, Mark
Structure and Evolution of Pre-Main Sequence Stars
title Structure and Evolution of Pre-Main Sequence Stars
title_full Structure and Evolution of Pre-Main Sequence Stars
title_fullStr Structure and Evolution of Pre-Main Sequence Stars
title_full_unstemmed Structure and Evolution of Pre-Main Sequence Stars
title_short Structure and Evolution of Pre-Main Sequence Stars
title_sort structure and evolution of pre main sequence stars
url http://hdl.handle.net/1721.1/77613
https://orcid.org/0000-0001-6932-2612
https://orcid.org/0000-0002-1379-4482
https://orcid.org/0000-0002-5769-8441
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