X-ray resonance scattering in a spherically symmetric coronal model
| ISSN: |
1573-093X
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|---|---|
| Source: |
Springer Online Journal Archives 1860-2000
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| Topics: |
Physics
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| Notes: |
Abstract In the solar corona the opacities of some of the prominent X-ray emission lines are on the order of τ ≈ 1 over typical coronal path lengths. We present and discuss a particular solution of the radiative transfer problem involving an extended, spherically symmetric coronal shell radiating isotropic, homogeneous emission in which single-scattering also takes place. Within the context of this simplified model we find that scattered radiation is an important contribution to the total emergent resonance line flux and that for the He-like family of resonance (r), intercombination (i), and forbidden (f) lines, the ratio G=(f + i)/r would decrease as a function of optical depth for disk-center emission in an extended spherically symmetric corona.
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| Type of Medium: |
Electronic Resource
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| URL: |
| _version_ | 1798296584177319937 |
|---|---|
| autor | Haisch, Bernhard M. Claflin, E. Scott |
| autorsonst | Haisch, Bernhard M. Claflin, E. Scott |
| book_url | http://dx.doi.org/10.1007/BF00157301 |
| datenlieferant | nat_lic_papers |
| hauptsatz | hsatz_simple |
| identnr | NLM195907116 |
| issn | 1573-093X |
| journal_name | Solar physics |
| materialart | 1 |
| notes | Abstract In the solar corona the opacities of some of the prominent X-ray emission lines are on the order of τ ≈ 1 over typical coronal path lengths. We present and discuss a particular solution of the radiative transfer problem involving an extended, spherically symmetric coronal shell radiating isotropic, homogeneous emission in which single-scattering also takes place. Within the context of this simplified model we find that scattered radiation is an important contribution to the total emergent resonance line flux and that for the He-like family of resonance (r), intercombination (i), and forbidden (f) lines, the ratio G=(f + i)/r would decrease as a function of optical depth for disk-center emission in an extended spherically symmetric corona. |
| package_name | Springer |
| publikationsjahr_anzeige | 1985 |
| publikationsjahr_facette | 1985 |
| publikationsjahr_intervall | 8014:1985-1989 |
| publikationsjahr_sort | 1985 |
| publisher | Springer |
| reference | 99 (1985), S. 101-109 |
| search_space | articles |
| shingle_author_1 | Haisch, Bernhard M. Claflin, E. Scott |
| shingle_author_2 | Haisch, Bernhard M. Claflin, E. Scott |
| shingle_author_3 | Haisch, Bernhard M. Claflin, E. Scott |
| shingle_author_4 | Haisch, Bernhard M. Claflin, E. Scott |
| shingle_catch_all_1 | Haisch, Bernhard M. Claflin, E. Scott X-ray resonance scattering in a spherically symmetric coronal model Abstract In the solar corona the opacities of some of the prominent X-ray emission lines are on the order of τ ≈ 1 over typical coronal path lengths. We present and discuss a particular solution of the radiative transfer problem involving an extended, spherically symmetric coronal shell radiating isotropic, homogeneous emission in which single-scattering also takes place. Within the context of this simplified model we find that scattered radiation is an important contribution to the total emergent resonance line flux and that for the He-like family of resonance (r), intercombination (i), and forbidden (f) lines, the ratio G=(f + i)/r would decrease as a function of optical depth for disk-center emission in an extended spherically symmetric corona. 1573-093X 1573093X Springer |
| shingle_catch_all_2 | Haisch, Bernhard M. Claflin, E. Scott X-ray resonance scattering in a spherically symmetric coronal model Abstract In the solar corona the opacities of some of the prominent X-ray emission lines are on the order of τ ≈ 1 over typical coronal path lengths. We present and discuss a particular solution of the radiative transfer problem involving an extended, spherically symmetric coronal shell radiating isotropic, homogeneous emission in which single-scattering also takes place. Within the context of this simplified model we find that scattered radiation is an important contribution to the total emergent resonance line flux and that for the He-like family of resonance (r), intercombination (i), and forbidden (f) lines, the ratio G=(f + i)/r would decrease as a function of optical depth for disk-center emission in an extended spherically symmetric corona. 1573-093X 1573093X Springer |
| shingle_catch_all_3 | Haisch, Bernhard M. Claflin, E. Scott X-ray resonance scattering in a spherically symmetric coronal model Abstract In the solar corona the opacities of some of the prominent X-ray emission lines are on the order of τ ≈ 1 over typical coronal path lengths. We present and discuss a particular solution of the radiative transfer problem involving an extended, spherically symmetric coronal shell radiating isotropic, homogeneous emission in which single-scattering also takes place. Within the context of this simplified model we find that scattered radiation is an important contribution to the total emergent resonance line flux and that for the He-like family of resonance (r), intercombination (i), and forbidden (f) lines, the ratio G=(f + i)/r would decrease as a function of optical depth for disk-center emission in an extended spherically symmetric corona. 1573-093X 1573093X Springer |
| shingle_catch_all_4 | Haisch, Bernhard M. Claflin, E. Scott X-ray resonance scattering in a spherically symmetric coronal model Abstract In the solar corona the opacities of some of the prominent X-ray emission lines are on the order of τ ≈ 1 over typical coronal path lengths. We present and discuss a particular solution of the radiative transfer problem involving an extended, spherically symmetric coronal shell radiating isotropic, homogeneous emission in which single-scattering also takes place. Within the context of this simplified model we find that scattered radiation is an important contribution to the total emergent resonance line flux and that for the He-like family of resonance (r), intercombination (i), and forbidden (f) lines, the ratio G=(f + i)/r would decrease as a function of optical depth for disk-center emission in an extended spherically symmetric corona. 1573-093X 1573093X Springer |
| shingle_title_1 | X-ray resonance scattering in a spherically symmetric coronal model |
| shingle_title_2 | X-ray resonance scattering in a spherically symmetric coronal model |
| shingle_title_3 | X-ray resonance scattering in a spherically symmetric coronal model |
| shingle_title_4 | X-ray resonance scattering in a spherically symmetric coronal model |
| sigel_instance_filter | dkfz geomar wilbert ipn albert fhp |
| source_archive | Springer Online Journal Archives 1860-2000 |
| timestamp | 2024-05-06T09:54:25.388Z |
| titel | X-ray resonance scattering in a spherically symmetric coronal model |
| titel_suche | X-ray resonance scattering in a spherically symmetric coronal model |
| topic | U |
| uid | nat_lic_papers_NLM195907116 |