A geomorphic analysis of Hale crater, Mars: The effects of impact into ice-rich crust

A. P. Jones, Alfred S. McEwen, L. L. Tornabene, Victor Baker, H. J. Melosh, D. C. Berman

Research output: Contribution to journalArticle

45 Citations (Scopus)

Abstract

Hale crater, a 125×150km impact crater located near the intersection of Uzboi Vallis and the northern rim of Argyre basin at 35.7°S, 323.6°E, is surrounded by channels that radiate from, incise, and transport material within Hale's ejecta. The spatial and temporal relationship between the channels and Hale's ejecta strongly suggests the impact event created or modified the channels and emplaced fluidized debris flow lobes over an extensive area (>200,000km2). We estimate ∼1010m3 of liquid water was required to form some of Hale's smaller channels, a volume we propose was supplied by subsurface ice melted and mobilized by the Hale-forming impact. If 10% of the subsurface volume was ice, based on a conservative porosity estimate for the upper martian crust, 1012m3 of liquid water could have been present in the ejecta. We determine a crater-retention age of 1Ga inside the primary cavity, providing a minimum age for Hale and a time at which we propose the subsurface was volatile-rich. Hale crater demonstrates the important role impacts may play in supplying liquid water to the martian surface: they are capable of producing fluvially-modified terrains that may be analogous to some landforms of Noachian Mars.

Original languageEnglish (US)
Pages (from-to)259-272
Number of pages14
JournalIcarus
Volume211
Issue number1
DOIs
StatePublished - Jan 1 2011

Fingerprint

Mars craters
craters
crater
Mars
crusts
ice
ejecta
crust
liquid
liquids
water
landforms
supplying
estimates
rims
debris
debris flow
lobes
mars
intersections

Keywords

  • Impact processes
  • Mars
  • Mars, Surface

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

A geomorphic analysis of Hale crater, Mars : The effects of impact into ice-rich crust. / Jones, A. P.; McEwen, Alfred S.; Tornabene, L. L.; Baker, Victor; Melosh, H. J.; Berman, D. C.

In: Icarus, Vol. 211, No. 1, 01.01.2011, p. 259-272.

Research output: Contribution to journalArticle

Jones, A. P. ; McEwen, Alfred S. ; Tornabene, L. L. ; Baker, Victor ; Melosh, H. J. ; Berman, D. C. / A geomorphic analysis of Hale crater, Mars : The effects of impact into ice-rich crust. In: Icarus. 2011 ; Vol. 211, No. 1. pp. 259-272.
@article{cbf1cae80e4049f2bbfef5151e0e60e7,
title = "A geomorphic analysis of Hale crater, Mars: The effects of impact into ice-rich crust",
abstract = "Hale crater, a 125×150km impact crater located near the intersection of Uzboi Vallis and the northern rim of Argyre basin at 35.7°S, 323.6°E, is surrounded by channels that radiate from, incise, and transport material within Hale's ejecta. The spatial and temporal relationship between the channels and Hale's ejecta strongly suggests the impact event created or modified the channels and emplaced fluidized debris flow lobes over an extensive area (>200,000km2). We estimate ∼1010m3 of liquid water was required to form some of Hale's smaller channels, a volume we propose was supplied by subsurface ice melted and mobilized by the Hale-forming impact. If 10{\%} of the subsurface volume was ice, based on a conservative porosity estimate for the upper martian crust, 1012m3 of liquid water could have been present in the ejecta. We determine a crater-retention age of 1Ga inside the primary cavity, providing a minimum age for Hale and a time at which we propose the subsurface was volatile-rich. Hale crater demonstrates the important role impacts may play in supplying liquid water to the martian surface: they are capable of producing fluvially-modified terrains that may be analogous to some landforms of Noachian Mars.",
keywords = "Impact processes, Mars, Mars, Surface",
author = "Jones, {A. P.} and McEwen, {Alfred S.} and Tornabene, {L. L.} and Victor Baker and Melosh, {H. J.} and Berman, {D. C.}",
year = "2011",
month = "1",
day = "1",
doi = "10.1016/j.icarus.2010.10.014",
language = "English (US)",
volume = "211",
pages = "259--272",
journal = "Icarus",
issn = "0019-1035",
publisher = "Academic Press Inc.",
number = "1",

}

TY - JOUR

T1 - A geomorphic analysis of Hale crater, Mars

T2 - The effects of impact into ice-rich crust

AU - Jones, A. P.

AU - McEwen, Alfred S.

AU - Tornabene, L. L.

AU - Baker, Victor

AU - Melosh, H. J.

AU - Berman, D. C.

PY - 2011/1/1

Y1 - 2011/1/1

N2 - Hale crater, a 125×150km impact crater located near the intersection of Uzboi Vallis and the northern rim of Argyre basin at 35.7°S, 323.6°E, is surrounded by channels that radiate from, incise, and transport material within Hale's ejecta. The spatial and temporal relationship between the channels and Hale's ejecta strongly suggests the impact event created or modified the channels and emplaced fluidized debris flow lobes over an extensive area (>200,000km2). We estimate ∼1010m3 of liquid water was required to form some of Hale's smaller channels, a volume we propose was supplied by subsurface ice melted and mobilized by the Hale-forming impact. If 10% of the subsurface volume was ice, based on a conservative porosity estimate for the upper martian crust, 1012m3 of liquid water could have been present in the ejecta. We determine a crater-retention age of 1Ga inside the primary cavity, providing a minimum age for Hale and a time at which we propose the subsurface was volatile-rich. Hale crater demonstrates the important role impacts may play in supplying liquid water to the martian surface: they are capable of producing fluvially-modified terrains that may be analogous to some landforms of Noachian Mars.

AB - Hale crater, a 125×150km impact crater located near the intersection of Uzboi Vallis and the northern rim of Argyre basin at 35.7°S, 323.6°E, is surrounded by channels that radiate from, incise, and transport material within Hale's ejecta. The spatial and temporal relationship between the channels and Hale's ejecta strongly suggests the impact event created or modified the channels and emplaced fluidized debris flow lobes over an extensive area (>200,000km2). We estimate ∼1010m3 of liquid water was required to form some of Hale's smaller channels, a volume we propose was supplied by subsurface ice melted and mobilized by the Hale-forming impact. If 10% of the subsurface volume was ice, based on a conservative porosity estimate for the upper martian crust, 1012m3 of liquid water could have been present in the ejecta. We determine a crater-retention age of 1Ga inside the primary cavity, providing a minimum age for Hale and a time at which we propose the subsurface was volatile-rich. Hale crater demonstrates the important role impacts may play in supplying liquid water to the martian surface: they are capable of producing fluvially-modified terrains that may be analogous to some landforms of Noachian Mars.

KW - Impact processes

KW - Mars

KW - Mars, Surface

UR - http://www.scopus.com/inward/record.url?scp=78650929588&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=78650929588&partnerID=8YFLogxK

U2 - 10.1016/j.icarus.2010.10.014

DO - 10.1016/j.icarus.2010.10.014

M3 - Article

AN - SCOPUS:78650929588

VL - 211

SP - 259

EP - 272

JO - Icarus

JF - Icarus

SN - 0019-1035

IS - 1

ER -