Computer Science
Scientific paper
Jul 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007hst..prop11116s&link_type=abstract
HST Proposal ID #11116. Cycle 16
Computer Science
Scientific paper
Stellar magnetic activity derives from the so-called "dynamo," a hydromagnetic interplay between overturning plasma motions and differential rotation in stars cool enough to support significant surface convection zones. The magnetic fields resulting from dynamo action are in turn are responsible for a wide range of high-energy emissions, including the spectacular outbursts called flares. Dynamo powered magnetic activity is not confined solely to stars, but also must occur, for example, in accretion disks of all descriptions, and in some planets. A great deal is known about magnetic activity in middle-aged G dwarfs like our Sun, thanks to its proximity. Less is known, however, about the much younger stars, newly emerged from the T-Tauri stage. Yet, it is during this phase that they reach the peak of their magnetic activity, and subsidiary influences, such as the impact of ionizing radiation and strong coronal winds on developing solar systems, also are maximum. One of the key missing ingredients in our current understanding are measurements of FUV emissions of such stars, to complement the extensive collections of coronal 1-10 MK X-ray measurements, particularly from recent ROSAT, Chandra and XMM-Newton surveys. We propose to conduct sensitive ACS/SBC prism ultraviolet spectroscopy of selected fields in two young 30 Myr Galactic clusters--IC 2391 and IC 2602--to inventory the key C IV emission index ~0.1 MK over a much larger and more diverse sample of coeval objects than has been possible hitherto. A key question is whether the FUV emissions also suffer the "saturation" and "super-saturation" at short rotation periods seen in coronal X-rays, or whether they continue to rise in the fastest rotating stars. The saturation behavior of the different temperature regimes holds important clues to the organization of the surface active regions on these very young stars, and should allow us to distinguish among several competing models.;
No associations
LandOfFree
Exploring the Early FUV History of Cool Stars: Transition Regions at 30 Myr does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Exploring the Early FUV History of Cool Stars: Transition Regions at 30 Myr, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Exploring the Early FUV History of Cool Stars: Transition Regions at 30 Myr will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-780502