MARC details
| 000 -LEADER |
|---|
| fixed length control field |
03418ctm a2200337Ia 4500 |
| 001 - CONTROL NUMBER |
|---|
| control field |
ocm43732089 |
| 003 - CONTROL NUMBER IDENTIFIER |
|---|
| control field |
OCoLC |
| 005 - DATE AND TIME OF LATEST TRANSACTION |
|---|
| control field |
20250219154102.0 |
| 008 - FIXED-LENGTH DATA ELEMENTS--GENERAL INFORMATION |
|---|
| fixed length control field |
000329s1999 xx a bm 000 0 eng d |
| 040 ## - CATALOGING SOURCE |
|---|
| Original cataloging agency |
COD |
| Transcribing agency |
COD |
| 049 ## - LOCAL HOLDINGS (OCLC) |
|---|
| Holding library |
CNRM |
| 090 ## - LOCALLY ASSIGNED LC-TYPE CALL NUMBER (OCLC); LOCAL CALL NUMBER (RLIN) |
|---|
| Classification number (OCLC) (R) ; Classification number, CALL (RLIN) (NR) |
QB523 .B174 1999 |
| 100 1# - MAIN ENTRY--PERSONAL NAME |
|---|
| Personal name |
Balch, Christopher C. |
| Fuller form of name |
(Christopher Connor) |
| 110 ## - MAIN ENTRY--CORPORATE NAME |
|---|
| Corporate name or jurisdiction name as entry element |
National Center for Atmospheric Research (NCAR) |
| 245 10 - TITLE STATEMENT |
|---|
| Title |
Energy analysis of post mass ejection solar coronal x-ray loops. |
| 264 ## - PRODUCTION, PUBLICATION, DISTRIBUTION, MANUFACTURE, AND COPYRIGHT NOTICE |
|---|
| Place of production, publication, distribution, manufacture |
Boulder, CO : |
| Name of producer, publisher, distributor, manufacturer |
National Center for Atmospheric Research (NCAR), |
| Date of production, publication, distribution, manufacture, or copyright notice |
1999. |
| 300 ## - PHYSICAL DESCRIPTION |
|---|
| Extent |
xxii, 344 leaves : |
| Other physical details |
ill. ; |
| Dimensions |
28 cm. |
| 336 ## - CONTENT TYPE |
|---|
| Content type term |
text |
| Content type code |
txt |
| Source |
rdacontent |
| 337 ## - MEDIA TYPE |
|---|
| Media type term |
unmediated |
| Media type code |
n |
| Source |
rdamedia |
| 338 ## - CARRIER TYPE |
|---|
| Carrier type term |
volume |
| Carrier type code |
nc |
| Source |
rdacarrier |
| 502 ## - DISSERTATION NOTE |
|---|
| Dissertation note |
Thesis (Ph. D.)--University of Colorado, 1999. |
| 504 ## - BIBLIOGRAPHY, ETC. NOTE |
|---|
| Bibliography, etc |
Includes bibliographical references (leaves 301-311). |
| 520 ## - SUMMARY, ETC. |
|---|
| Summary, etc. |
Solar coronal mass ejections have been shown in the past to be associated with the enhancement of solar x-ray emission of several hours duration. Analysis of solar x-ray images has shown that these long-duration x-ray events are due to an arcade of post mass ejection loops that form over the magnetic polarity inversion line that lies underneath the mass ejections. While this has been successfully described qualitatively in past work, we seek to apply a quantitative analysis to understand the detailed evolution of energy balance in the system, including the evolution of heating and cooling mechanisms We measured a set of intensity-time profiles as a function of height for particularly well observed arcade events on the solar limb with relatively simple morphology. We developed a semi-theoretical model, with the basic premise that at each point in space, the intensity is the response to an interplay between a source term and a cooling term. This principle is developed for models with increasingly sophisticated geometries in order to test the effect of line-of-sight integration of x-ray emission in the image data. The models for the data are expressed in terms of a set of free parameters, which are then optimized to provide the best fit of the model to the data. Our best-fit parameters enable us to make several inferences about the physical nature of the system. The region of heating develops early in the event and spans a surprisingly large vertical dimension. The heating continues throughout much of the duration of the event. The enhancement of x-ray emission is primarily due to an enhancement of density of plasma in the loops, although there is a small increase in temperature. During the early phase of the event, radiative and conductive cooling are of similar magnitude, but increase more slowly than heating. Once the cooling mechanisms surpass heating the event enters the cooling phase. During this phase, the radiative cooling decreases relatively quickly and conductive cooling becomes the dominant cooling mechanism. We compare the energy of the heating with the energies of an approximate model for the coronal magnetic field to make an estimate of the energy released by magnetic reconnection. |
| 610 ## - SUBJECT ADDED ENTRY--CORPORATE NAME |
|---|
| Corporate name or jurisdiction name as entry element |
National Center for Atmospheric Research (NCAR) |
| 650 #0 - SUBJECT ADDED ENTRY--TOPICAL TERM |
|---|
| Topical term or geographic name as entry element |
Solar flares |
| General subdivision |
Observations. |
| 650 #0 - SUBJECT ADDED ENTRY--TOPICAL TERM |
|---|
| Topical term or geographic name as entry element |
X-ray astronomy. |
| 651 #0 - SUBJECT ADDED ENTRY--GEOGRAPHIC NAME |
|---|
| Geographic name |
Sun |
| General subdivision |
Loop prominences. |
| 710 ## - ADDED ENTRY--CORPORATE NAME |
|---|
| Corporate name or jurisdiction name as entry element |
National Center for Atmospheric Research (NCAR) |
| 830 ## - SERIES ADDED ENTRY--UNIFORM TITLE |
|---|
| Uniform title |
NCAR Cooperative Thesis ; |
| Volume number/sequential designation |
166 |
| 942 ## - ADDED ENTRY ELEMENTS (KOHA) |
|---|
| Koha item type |
BOOK |
| Source of classification or shelving scheme |
Library of Congress Classification |
