The Jovian stratosphere in the ultraviolet
Wagener, R. ; Caldwell, J. ; Owen, T. ; Sang-Joon Kim ; Encrenaz, T. ; Combes, M.
Amsterdam : Elsevier
Amsterdam : Elsevier
| ISSN: |
0019-1035
|
|---|---|
| Source: |
Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
|
| Topics: |
Physics
|
| Type of Medium: |
Electronic Resource
|
| URL: |
| _version_ | 1798290858087284736 |
|---|---|
| autor | Wagener, R. Caldwell, J. Owen, T. Sang-Joon Kim Encrenaz, T. Combes, M. |
| autorsonst | Wagener, R. Caldwell, J. Owen, T. Sang-Joon Kim Encrenaz, T. Combes, M. |
| book_url | http://dx.doi.org/10.1016/0019-1035(85)90007-7 |
| datenlieferant | nat_lic_papers |
| fussnote | The center-of-disk reflectivity of Jupiter in the wavelength range from 1450 to 3150 A has been computed from 30 low-dispersion IUE spectra taken during solar maximum in 1978-1980. A vertically inhomogeneous radiative transfer program is used to compute model reflectivities of various stratospheric compositions for comparison. Ammonia and acetylene are well determined because they show narrow absorption bands in the ultraviolet. Above 1800 A, these two gases provide a good fit to the data, but not below. At shorter wavelengths the fit would be much improved by a small amount (5-15 ppb) of propadiene/allene (C"3H"4). Voyager IRIS spectra show that the IR bands of allene are not strong enough to be detected in such a small amount. Additional absorption around 1600 A can be reproduced best with the presence of cyclopropane (C"3H"6, 〈15 ppb), although other absorbers (e.g., hydrocarbon molecules with more than three carbon atoms, oxygen- or nitrogen-containing molecules, or a high-attitude haze) could also explain the spectrum in this region. The data are too noisy to detect possible CO Cameron band absorption near 2000 A. |
| hauptsatz | hsatz_simple |
| identnr | NLZ180407430 |
| issn | 0019-1035 |
| journal_name | Icarus |
| materialart | 1 |
| package_name | Elsevier |
| publikationsort | Amsterdam |
| publisher | Elsevier |
| reference | 63 (1985), S. 222-236 |
| search_space | articles |
| shingle_author_1 | Wagener, R. Caldwell, J. Owen, T. Sang-Joon Kim Encrenaz, T. Combes, M. |
| shingle_author_2 | Wagener, R. Caldwell, J. Owen, T. Sang-Joon Kim Encrenaz, T. Combes, M. |
| shingle_author_3 | Wagener, R. Caldwell, J. Owen, T. Sang-Joon Kim Encrenaz, T. Combes, M. |
| shingle_author_4 | Wagener, R. Caldwell, J. Owen, T. Sang-Joon Kim Encrenaz, T. Combes, M. |
| shingle_catch_all_1 | Wagener, R. Caldwell, J. Owen, T. Sang-Joon Kim Encrenaz, T. Combes, M. The Jovian stratosphere in the ultraviolet 0019-1035 00191035 Elsevier |
| shingle_catch_all_2 | Wagener, R. Caldwell, J. Owen, T. Sang-Joon Kim Encrenaz, T. Combes, M. The Jovian stratosphere in the ultraviolet 0019-1035 00191035 Elsevier |
| shingle_catch_all_3 | Wagener, R. Caldwell, J. Owen, T. Sang-Joon Kim Encrenaz, T. Combes, M. The Jovian stratosphere in the ultraviolet 0019-1035 00191035 Elsevier |
| shingle_catch_all_4 | Wagener, R. Caldwell, J. Owen, T. Sang-Joon Kim Encrenaz, T. Combes, M. The Jovian stratosphere in the ultraviolet 0019-1035 00191035 Elsevier |
| shingle_title_1 | The Jovian stratosphere in the ultraviolet |
| shingle_title_2 | The Jovian stratosphere in the ultraviolet |
| shingle_title_3 | The Jovian stratosphere in the ultraviolet |
| shingle_title_4 | The Jovian stratosphere in the ultraviolet |
| sigel_instance_filter | dkfz geomar wilbert ipn albert fhp |
| source_archive | Elsevier Journal Backfiles on ScienceDirect 1907 - 2002 |
| timestamp | 2024-05-06T08:23:24.636Z |
| titel | The Jovian stratosphere in the ultraviolet |
| titel_suche | The Jovian stratosphere in the ultraviolet The center-of-disk reflectivity of Jupiter in the wavelength range from 1450 to 3150 A has been computed from 30 low-dispersion IUE spectra taken during solar maximum in 1978-1980. A vertically inhomogeneous radiative transfer program is used to compute model reflectivities of various stratospheric compositions for comparison. Ammonia and acetylene are well determined because they show narrow absorption bands in the ultraviolet. Above 1800 A, these two gases provide a good fit to the data, but not below. At shorter wavelengths the fit would be much improved by a small amount (5-15 ppb) of propadiene/allene (C"3H"4). Voyager IRIS spectra show that the IR bands of allene are not strong enough to be detected in such a small amount. Additional absorption around 1600 A can be reproduced best with the presence of cyclopropane (C"3H"6, 〈15 ppb), although other absorbers (e.g., hydrocarbon molecules with more than three carbon atoms, oxygen- or nitrogen-containing molecules, or a high-attitude haze) could also explain the spectrum in this region. The data are too noisy to detect possible CO Cameron band absorption near 2000 A. |
| topic | U |
| uid | nat_lic_papers_NLZ180407430 |