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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National Academy of Sciences
2013
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| Online Zugang: | 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. |
| first_indexed | 2024-09-23T12:34:52Z |
| format | Article |
| id | mit-1721.1/77613 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T12:34:52Z |
| publishDate | 2013 |
| publisher | National Academy of Sciences |
| record_format | dspace |
| 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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