Evidence for Amazonian highly viscous lavas in the southern highlands on Mars
We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Brož, Petr [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2015transfer abstract |
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| Schlagwörter: |
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| Umfang: |
13 |
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| Übergeordnetes Werk: |
Enthalten in: Energy consumption and environmental degradation nexus: A systematic review and meta-analysis of fossil fuel and renewable energy consumption - Kılıç Depren, Serpil ELSEVIER, 2022, Amsterdam [u.a.] |
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| Übergeordnetes Werk: |
volume:415 ; year:2015 ; day:1 ; month:04 ; pages:200-212 ; extent:13 |
| Links: |
|---|
| DOI / URN: |
10.1016/j.epsl.2015.01.033 |
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ELV023945621 |
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| 520 | |a We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that these features were formed by volcanic activity of viscous lavas in the mid-Amazonian epoch, relatively recently in martian history. If our hypothesis is correct, this small volcanic field represents rare evidence of young volcanic activity in the martian highlands in which martian equivalents of terrestrial lava domes and coulées might be present. On Earth, such landforms are usually formed by highly viscous evolved lavas, i.e., andesitic to rhyolitic, for which observational evidence is sparse on Mars. Hence, this field might be one of only a few where martian evolved lavas might be investigated in detail. | ||
| 520 | |a We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that these features were formed by volcanic activity of viscous lavas in the mid-Amazonian epoch, relatively recently in martian history. If our hypothesis is correct, this small volcanic field represents rare evidence of young volcanic activity in the martian highlands in which martian equivalents of terrestrial lava domes and coulées might be present. On Earth, such landforms are usually formed by highly viscous evolved lavas, i.e., andesitic to rhyolitic, for which observational evidence is sparse on Mars. Hence, this field might be one of only a few where martian evolved lavas might be investigated in detail. | ||
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10.1016/j.epsl.2015.01.033 doi GBVA2015021000002.pica (DE-627)ELV023945621 (ELSEVIER)S0012-821X(15)00061-8 DE-627 ger DE-627 rakwb eng 550 550 DE-600 610 333.7 VZ BIODIV DE-30 fid 42.90 bkl 42.11 bkl Brož, Petr verfasserin aut Evidence for Amazonian highly viscous lavas in the southern highlands on Mars 2015transfer abstract 13 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that these features were formed by volcanic activity of viscous lavas in the mid-Amazonian epoch, relatively recently in martian history. If our hypothesis is correct, this small volcanic field represents rare evidence of young volcanic activity in the martian highlands in which martian equivalents of terrestrial lava domes and coulées might be present. On Earth, such landforms are usually formed by highly viscous evolved lavas, i.e., andesitic to rhyolitic, for which observational evidence is sparse on Mars. Hence, this field might be one of only a few where martian evolved lavas might be investigated in detail. We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that these features were formed by volcanic activity of viscous lavas in the mid-Amazonian epoch, relatively recently in martian history. If our hypothesis is correct, this small volcanic field represents rare evidence of young volcanic activity in the martian highlands in which martian equivalents of terrestrial lava domes and coulées might be present. On Earth, such landforms are usually formed by highly viscous evolved lavas, i.e., andesitic to rhyolitic, for which observational evidence is sparse on Mars. Hence, this field might be one of only a few where martian evolved lavas might be investigated in detail. Mars Elsevier Mars surface Elsevier lava dome Elsevier volcanism Elsevier Hauber, Ernst oth Platz, Thomas oth Balme, Matt oth Enthalten in Elsevier Kılıç Depren, Serpil ELSEVIER Energy consumption and environmental degradation nexus: A systematic review and meta-analysis of fossil fuel and renewable energy consumption 2022 Amsterdam [u.a.] (DE-627)ELV008390509 volume:415 year:2015 day:1 month:04 pages:200-212 extent:13 https://doi.org/10.1016/j.epsl.2015.01.033 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U FID-BIODIV SSG-OLC-PHA 42.90 Ökologie: Allgemeines VZ 42.11 Biomathematik Biokybernetik VZ AR 415 2015 1 0401 200-212 13 045F 550 |
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10.1016/j.epsl.2015.01.033 doi GBVA2015021000002.pica (DE-627)ELV023945621 (ELSEVIER)S0012-821X(15)00061-8 DE-627 ger DE-627 rakwb eng 550 550 DE-600 610 333.7 VZ BIODIV DE-30 fid 42.90 bkl 42.11 bkl Brož, Petr verfasserin aut Evidence for Amazonian highly viscous lavas in the southern highlands on Mars 2015transfer abstract 13 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that these features were formed by volcanic activity of viscous lavas in the mid-Amazonian epoch, relatively recently in martian history. If our hypothesis is correct, this small volcanic field represents rare evidence of young volcanic activity in the martian highlands in which martian equivalents of terrestrial lava domes and coulées might be present. On Earth, such landforms are usually formed by highly viscous evolved lavas, i.e., andesitic to rhyolitic, for which observational evidence is sparse on Mars. Hence, this field might be one of only a few where martian evolved lavas might be investigated in detail. We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that these features were formed by volcanic activity of viscous lavas in the mid-Amazonian epoch, relatively recently in martian history. If our hypothesis is correct, this small volcanic field represents rare evidence of young volcanic activity in the martian highlands in which martian equivalents of terrestrial lava domes and coulées might be present. On Earth, such landforms are usually formed by highly viscous evolved lavas, i.e., andesitic to rhyolitic, for which observational evidence is sparse on Mars. Hence, this field might be one of only a few where martian evolved lavas might be investigated in detail. Mars Elsevier Mars surface Elsevier lava dome Elsevier volcanism Elsevier Hauber, Ernst oth Platz, Thomas oth Balme, Matt oth Enthalten in Elsevier Kılıç Depren, Serpil ELSEVIER Energy consumption and environmental degradation nexus: A systematic review and meta-analysis of fossil fuel and renewable energy consumption 2022 Amsterdam [u.a.] (DE-627)ELV008390509 volume:415 year:2015 day:1 month:04 pages:200-212 extent:13 https://doi.org/10.1016/j.epsl.2015.01.033 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U FID-BIODIV SSG-OLC-PHA 42.90 Ökologie: Allgemeines VZ 42.11 Biomathematik Biokybernetik VZ AR 415 2015 1 0401 200-212 13 045F 550 |
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10.1016/j.epsl.2015.01.033 doi GBVA2015021000002.pica (DE-627)ELV023945621 (ELSEVIER)S0012-821X(15)00061-8 DE-627 ger DE-627 rakwb eng 550 550 DE-600 610 333.7 VZ BIODIV DE-30 fid 42.90 bkl 42.11 bkl Brož, Petr verfasserin aut Evidence for Amazonian highly viscous lavas in the southern highlands on Mars 2015transfer abstract 13 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that these features were formed by volcanic activity of viscous lavas in the mid-Amazonian epoch, relatively recently in martian history. If our hypothesis is correct, this small volcanic field represents rare evidence of young volcanic activity in the martian highlands in which martian equivalents of terrestrial lava domes and coulées might be present. On Earth, such landforms are usually formed by highly viscous evolved lavas, i.e., andesitic to rhyolitic, for which observational evidence is sparse on Mars. Hence, this field might be one of only a few where martian evolved lavas might be investigated in detail. We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that these features were formed by volcanic activity of viscous lavas in the mid-Amazonian epoch, relatively recently in martian history. If our hypothesis is correct, this small volcanic field represents rare evidence of young volcanic activity in the martian highlands in which martian equivalents of terrestrial lava domes and coulées might be present. On Earth, such landforms are usually formed by highly viscous evolved lavas, i.e., andesitic to rhyolitic, for which observational evidence is sparse on Mars. Hence, this field might be one of only a few where martian evolved lavas might be investigated in detail. Mars Elsevier Mars surface Elsevier lava dome Elsevier volcanism Elsevier Hauber, Ernst oth Platz, Thomas oth Balme, Matt oth Enthalten in Elsevier Kılıç Depren, Serpil ELSEVIER Energy consumption and environmental degradation nexus: A systematic review and meta-analysis of fossil fuel and renewable energy consumption 2022 Amsterdam [u.a.] (DE-627)ELV008390509 volume:415 year:2015 day:1 month:04 pages:200-212 extent:13 https://doi.org/10.1016/j.epsl.2015.01.033 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U FID-BIODIV SSG-OLC-PHA 42.90 Ökologie: Allgemeines VZ 42.11 Biomathematik Biokybernetik VZ AR 415 2015 1 0401 200-212 13 045F 550 |
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10.1016/j.epsl.2015.01.033 doi GBVA2015021000002.pica (DE-627)ELV023945621 (ELSEVIER)S0012-821X(15)00061-8 DE-627 ger DE-627 rakwb eng 550 550 DE-600 610 333.7 VZ BIODIV DE-30 fid 42.90 bkl 42.11 bkl Brož, Petr verfasserin aut Evidence for Amazonian highly viscous lavas in the southern highlands on Mars 2015transfer abstract 13 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that these features were formed by volcanic activity of viscous lavas in the mid-Amazonian epoch, relatively recently in martian history. If our hypothesis is correct, this small volcanic field represents rare evidence of young volcanic activity in the martian highlands in which martian equivalents of terrestrial lava domes and coulées might be present. On Earth, such landforms are usually formed by highly viscous evolved lavas, i.e., andesitic to rhyolitic, for which observational evidence is sparse on Mars. Hence, this field might be one of only a few where martian evolved lavas might be investigated in detail. We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that these features were formed by volcanic activity of viscous lavas in the mid-Amazonian epoch, relatively recently in martian history. If our hypothesis is correct, this small volcanic field represents rare evidence of young volcanic activity in the martian highlands in which martian equivalents of terrestrial lava domes and coulées might be present. On Earth, such landforms are usually formed by highly viscous evolved lavas, i.e., andesitic to rhyolitic, for which observational evidence is sparse on Mars. Hence, this field might be one of only a few where martian evolved lavas might be investigated in detail. Mars Elsevier Mars surface Elsevier lava dome Elsevier volcanism Elsevier Hauber, Ernst oth Platz, Thomas oth Balme, Matt oth Enthalten in Elsevier Kılıç Depren, Serpil ELSEVIER Energy consumption and environmental degradation nexus: A systematic review and meta-analysis of fossil fuel and renewable energy consumption 2022 Amsterdam [u.a.] (DE-627)ELV008390509 volume:415 year:2015 day:1 month:04 pages:200-212 extent:13 https://doi.org/10.1016/j.epsl.2015.01.033 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U FID-BIODIV SSG-OLC-PHA 42.90 Ökologie: Allgemeines VZ 42.11 Biomathematik Biokybernetik VZ AR 415 2015 1 0401 200-212 13 045F 550 |
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10.1016/j.epsl.2015.01.033 doi GBVA2015021000002.pica (DE-627)ELV023945621 (ELSEVIER)S0012-821X(15)00061-8 DE-627 ger DE-627 rakwb eng 550 550 DE-600 610 333.7 VZ BIODIV DE-30 fid 42.90 bkl 42.11 bkl Brož, Petr verfasserin aut Evidence for Amazonian highly viscous lavas in the southern highlands on Mars 2015transfer abstract 13 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that these features were formed by volcanic activity of viscous lavas in the mid-Amazonian epoch, relatively recently in martian history. If our hypothesis is correct, this small volcanic field represents rare evidence of young volcanic activity in the martian highlands in which martian equivalents of terrestrial lava domes and coulées might be present. On Earth, such landforms are usually formed by highly viscous evolved lavas, i.e., andesitic to rhyolitic, for which observational evidence is sparse on Mars. Hence, this field might be one of only a few where martian evolved lavas might be investigated in detail. We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that these features were formed by volcanic activity of viscous lavas in the mid-Amazonian epoch, relatively recently in martian history. If our hypothesis is correct, this small volcanic field represents rare evidence of young volcanic activity in the martian highlands in which martian equivalents of terrestrial lava domes and coulées might be present. On Earth, such landforms are usually formed by highly viscous evolved lavas, i.e., andesitic to rhyolitic, for which observational evidence is sparse on Mars. Hence, this field might be one of only a few where martian evolved lavas might be investigated in detail. Mars Elsevier Mars surface Elsevier lava dome Elsevier volcanism Elsevier Hauber, Ernst oth Platz, Thomas oth Balme, Matt oth Enthalten in Elsevier Kılıç Depren, Serpil ELSEVIER Energy consumption and environmental degradation nexus: A systematic review and meta-analysis of fossil fuel and renewable energy consumption 2022 Amsterdam [u.a.] (DE-627)ELV008390509 volume:415 year:2015 day:1 month:04 pages:200-212 extent:13 https://doi.org/10.1016/j.epsl.2015.01.033 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U FID-BIODIV SSG-OLC-PHA 42.90 Ökologie: Allgemeines VZ 42.11 Biomathematik Biokybernetik VZ AR 415 2015 1 0401 200-212 13 045F 550 |
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Enthalten in Energy consumption and environmental degradation nexus: A systematic review and meta-analysis of fossil fuel and renewable energy consumption Amsterdam [u.a.] volume:415 year:2015 day:1 month:04 pages:200-212 extent:13 |
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Enthalten in Energy consumption and environmental degradation nexus: A systematic review and meta-analysis of fossil fuel and renewable energy consumption Amsterdam [u.a.] volume:415 year:2015 day:1 month:04 pages:200-212 extent:13 |
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Energy consumption and environmental degradation nexus: A systematic review and meta-analysis of fossil fuel and renewable energy consumption |
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evidence for amazonian highly viscous lavas in the southern highlands on mars |
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Evidence for Amazonian highly viscous lavas in the southern highlands on Mars |
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We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that these features were formed by volcanic activity of viscous lavas in the mid-Amazonian epoch, relatively recently in martian history. If our hypothesis is correct, this small volcanic field represents rare evidence of young volcanic activity in the martian highlands in which martian equivalents of terrestrial lava domes and coulées might be present. On Earth, such landforms are usually formed by highly viscous evolved lavas, i.e., andesitic to rhyolitic, for which observational evidence is sparse on Mars. Hence, this field might be one of only a few where martian evolved lavas might be investigated in detail. |
| abstractGer |
We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that these features were formed by volcanic activity of viscous lavas in the mid-Amazonian epoch, relatively recently in martian history. If our hypothesis is correct, this small volcanic field represents rare evidence of young volcanic activity in the martian highlands in which martian equivalents of terrestrial lava domes and coulées might be present. On Earth, such landforms are usually formed by highly viscous evolved lavas, i.e., andesitic to rhyolitic, for which observational evidence is sparse on Mars. Hence, this field might be one of only a few where martian evolved lavas might be investigated in detail. |
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We have identified small-scale volcanic edifices, two cones and three domes with associated flows, within Terra Sirenum, a region situated in the martian southern highlands. Based on thermal, morphological, and morphometrical properties, and the determination of absolute model ages, we conclude that these features were formed by volcanic activity of viscous lavas in the mid-Amazonian epoch, relatively recently in martian history. If our hypothesis is correct, this small volcanic field represents rare evidence of young volcanic activity in the martian highlands in which martian equivalents of terrestrial lava domes and coulées might be present. On Earth, such landforms are usually formed by highly viscous evolved lavas, i.e., andesitic to rhyolitic, for which observational evidence is sparse on Mars. Hence, this field might be one of only a few where martian evolved lavas might be investigated in detail. |
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