The Martian paleoclimate and enhanced atmospheric carbon dioxide
| ISSN: |
0019-1035
|
|---|---|
| Source: |
Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
|
| Topics: |
Physics
|
| Type of Medium: |
Electronic Resource
|
| URL: |
| _version_ | 1798290857591308289 |
|---|---|
| autor | Cess, R.D. Ramanathan, V. Owen, T. |
| autorsonst | Cess, R.D. Ramanathan, V. Owen, T. |
| book_url | http://linkinghub.elsevier.com/retrieve/pii/0019-1035(80)90169-4 |
| datenlieferant | nat_lic_papers |
| fussnote | Current evidence indicates that the Martian surface is abundant with water presently in the form of ice, while the atmosphere was at one time more massive with a past surface pressure of as much as 1 atm of CO"2. In an attempt to understand the Martian paleoclimate, we have modeled a past CO"2H"2O greenhouse and find global temperatures which are consistent with an earlier presence of liquid surface water, a finding which agrees with the extensive evidence for past fluvial erosion. An important aspect of the CO"2H"2O greenhouse model is the detailed inclusion of CO"2 hot bands. For a surface pressure of 1 atm of CO"2, the present greenhouse model predicts a global mean surface temperature of 294^oK, but if the hot bands are excluded, a surface temperature of only 250^oK is achieved. |
| hauptsatz | hsatz_simple |
| identnr | NLZ180400061 |
| issn | 0019-1035 |
| journal_name | Icarus |
| materialart | 1 |
| package_name | Elsevier |
| publikationsort | Amsterdam |
| publisher | Elsevier |
| reference | 41 (1980), S. 159-165 |
| search_space | articles |
| shingle_author_1 | Cess, R.D. Ramanathan, V. Owen, T. |
| shingle_author_2 | Cess, R.D. Ramanathan, V. Owen, T. |
| shingle_author_3 | Cess, R.D. Ramanathan, V. Owen, T. |
| shingle_author_4 | Cess, R.D. Ramanathan, V. Owen, T. |
| shingle_catch_all_1 | Cess, R.D. Ramanathan, V. Owen, T. The Martian paleoclimate and enhanced atmospheric carbon dioxide 0019-1035 00191035 Elsevier |
| shingle_catch_all_2 | Cess, R.D. Ramanathan, V. Owen, T. The Martian paleoclimate and enhanced atmospheric carbon dioxide 0019-1035 00191035 Elsevier |
| shingle_catch_all_3 | Cess, R.D. Ramanathan, V. Owen, T. The Martian paleoclimate and enhanced atmospheric carbon dioxide 0019-1035 00191035 Elsevier |
| shingle_catch_all_4 | Cess, R.D. Ramanathan, V. Owen, T. The Martian paleoclimate and enhanced atmospheric carbon dioxide 0019-1035 00191035 Elsevier |
| shingle_title_1 | The Martian paleoclimate and enhanced atmospheric carbon dioxide |
| shingle_title_2 | The Martian paleoclimate and enhanced atmospheric carbon dioxide |
| shingle_title_3 | The Martian paleoclimate and enhanced atmospheric carbon dioxide |
| shingle_title_4 | The Martian paleoclimate and enhanced atmospheric carbon dioxide |
| sigel_instance_filter | dkfz geomar wilbert ipn albert fhp |
| source_archive | Elsevier Journal Backfiles on ScienceDirect 1907 - 2002 |
| timestamp | 2024-05-06T08:23:23.520Z |
| titel | The Martian paleoclimate and enhanced atmospheric carbon dioxide |
| titel_suche | The Martian paleoclimate and enhanced atmospheric carbon dioxide Current evidence indicates that the Martian surface is abundant with water presently in the form of ice, while the atmosphere was at one time more massive with a past surface pressure of as much as 1 atm of CO"2. In an attempt to understand the Martian paleoclimate, we have modeled a past CO"2H"2O greenhouse and find global temperatures which are consistent with an earlier presence of liquid surface water, a finding which agrees with the extensive evidence for past fluvial erosion. An important aspect of the CO"2H"2O greenhouse model is the detailed inclusion of CO"2 hot bands. For a surface pressure of 1 atm of CO"2, the present greenhouse model predicts a global mean surface temperature of 294^oK, but if the hot bands are excluded, a surface temperature of only 250^oK is achieved. |
| topic | U |
| uid | nat_lic_papers_NLZ180400061 |