Response timescales for martian ice masses and implications for ice flow on Mars

Research output: Contribution to journal › Journal article › Research › peer-review

Standard

Response timescales for martian ice masses and implications for ice flow on Mars. / Koutnik, Michelle Rebecca; Waddington, E.D.; Winebrener, D.P.; Pathare, A.S.

In: Icarus, Vol. 225, No. 2, 17.10.2013, p. 949-959.

Research output: Contribution to journal › Journal article › Research › peer-review

Harvard

Koutnik, MR, Waddington, ED, Winebrener, DP & Pathare, AS 2013, 'Response timescales for martian ice masses and implications for ice flow on Mars', Icarus, vol. 225, no. 2, pp. 949-959. < http://dx.doi.org/10.1016/j.icarus.2012.09.031>

APA

Koutnik, M. R., Waddington, E. D., Winebrener, D. P., & Pathare, A. S. (2013). Response timescales for martian ice masses and implications for ice flow on Mars. Icarus, 225(2), 949-959. http://dx.doi.org/10.1016/j.icarus.2012.09.031

Vancouver

Koutnik MR, Waddington ED, Winebrener DP, Pathare AS. Response timescales for martian ice masses and implications for ice flow on Mars. Icarus. 2013 Oct 17;225(2):949-959.

Author

Koutnik, Michelle Rebecca ; Waddington, E.D. ; Winebrener, D.P. ; Pathare, A.S. / Response timescales for martian ice masses and implications for ice flow on Mars. In: Icarus. 2013 ; Vol. 225, No. 2. pp. 949-959.

Bibtex

@article{53fc8d6a5e99487192398cabe3ef8583,
title = "Response timescales for martian ice masses and implications for ice flow on Mars",
abstract = "On Earth and on Mars, ice masses experience changes in precipitation, temperature, and radiation. In a new climate state, flowing ice masses will adjust in length and in thickness, and this response toward a new steady state has a characteristic timescale. However, a flowing ice mass has a predictable shape, which is a function of ice temperature, ice rheology, and surface mass-exchange rate. In addition, the time for surface-shape adjustment is shorter than the characteristic time for significant deformation or displacement of internal layers within a flowing ice mass; as a result, surface topography is more diagnostic of flow than are internal-layer shapes. Because the shape of Gemina Lingula, North Polar Layered Deposits indicates that it flowed at some time in the past, we use its current topography to infer characteristics of those past ice conditions, or past climate conditions, in which ice-flow rates were more significant than today. A plausible range of near-basal ice temperatures and ice-flow enhancement factors can generate the characteristic geometry of an ice mass that has been shaped by flow over reasonable volume-response timescales. All plausible ice-flow scenarios require conditions that are different from present-day Mars, if the basal layers are pure ice.",
author = "Koutnik, {Michelle Rebecca} and E.D. Waddington and D.P. Winebrener and A.S. Pathare",
year = "2013",
month = oct,
day = "17",
language = "English",
volume = "225",
pages = "949--959",
journal = "Icarus",
issn = "0019-1035",
publisher = "Elsevier",
number = "2",

}

RIS

TY - JOUR

T1 - Response timescales for martian ice masses and implications for ice flow on Mars

AU - Koutnik, Michelle Rebecca

AU - Waddington, E.D.

AU - Winebrener, D.P.

AU - Pathare, A.S.

PY - 2013/10/17

Y1 - 2013/10/17

N2 - On Earth and on Mars, ice masses experience changes in precipitation, temperature, and radiation. In a new climate state, flowing ice masses will adjust in length and in thickness, and this response toward a new steady state has a characteristic timescale. However, a flowing ice mass has a predictable shape, which is a function of ice temperature, ice rheology, and surface mass-exchange rate. In addition, the time for surface-shape adjustment is shorter than the characteristic time for significant deformation or displacement of internal layers within a flowing ice mass; as a result, surface topography is more diagnostic of flow than are internal-layer shapes. Because the shape of Gemina Lingula, North Polar Layered Deposits indicates that it flowed at some time in the past, we use its current topography to infer characteristics of those past ice conditions, or past climate conditions, in which ice-flow rates were more significant than today. A plausible range of near-basal ice temperatures and ice-flow enhancement factors can generate the characteristic geometry of an ice mass that has been shaped by flow over reasonable volume-response timescales. All plausible ice-flow scenarios require conditions that are different from present-day Mars, if the basal layers are pure ice.

AB - On Earth and on Mars, ice masses experience changes in precipitation, temperature, and radiation. In a new climate state, flowing ice masses will adjust in length and in thickness, and this response toward a new steady state has a characteristic timescale. However, a flowing ice mass has a predictable shape, which is a function of ice temperature, ice rheology, and surface mass-exchange rate. In addition, the time for surface-shape adjustment is shorter than the characteristic time for significant deformation or displacement of internal layers within a flowing ice mass; as a result, surface topography is more diagnostic of flow than are internal-layer shapes. Because the shape of Gemina Lingula, North Polar Layered Deposits indicates that it flowed at some time in the past, we use its current topography to infer characteristics of those past ice conditions, or past climate conditions, in which ice-flow rates were more significant than today. A plausible range of near-basal ice temperatures and ice-flow enhancement factors can generate the characteristic geometry of an ice mass that has been shaped by flow over reasonable volume-response timescales. All plausible ice-flow scenarios require conditions that are different from present-day Mars, if the basal layers are pure ice.

M3 - Journal article

VL - 225

SP - 949

EP - 959

JO - Icarus

JF - Icarus

SN - 0019-1035

IS - 2

ER -

ID: 43557255