H. Hoffmann

Planet

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Document Type

Co-Authors

G. Neukum

Freie Universität Berlin

R. Jaumann

Freie Universität Berlin

Ernst Hauber

Deutsches Zentrum für Luft- und Raumfahrt e. V. (DLR)

F. Scholten

Deutsches Zentrum für Luft- und Raumfahrt e. V. (DLR)

J. W. Head

Lancaster University

S. van Gasselt

National Chengchi University

T. Roatsch

Deutsches Zentrum für Luft- und Raumfahrt e. V. (DLR)

A. T. Basilevsky

Russian Academy of Sciences

Ph. Masson

Université Paris-Sud

F. Poulet

Institut d'Astrophysique Spatiale

Cooperative Institutions

Brown University

Planetary Science Institute

Centre National de la Recherche Scientifique

Deutsches Zentrum für Luft- und Raumfahrt e. V. (DLR)

Jet Propulsion Laboratory

Institut d'Astrophysique Spatiale

Planet

Campus France

Observatoire Midi-Pyrénées

Université Paris Cité

Author Statistics

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A Model of Spectral Albedo of Particulate Surfaces: Implications for Optical Properties of the Moon

Icarus (1999)

Yurij G. Shkuratov L. V. Starukhina H. Hoffmann G. Arnold

Regolith

Albedo (alchemy)

Pyroxene

Spectral slope

Single-scattering albedo

10.1006/icar.1998.6035

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Citations (432)

Mars Express High Resolution Stereo Camera spectrophotometric data: Characteristics and science analysis

Journal of Geophysical Research Atmospheres (2007)

T. B. McCord J. B. Adams G. Bellucci Jean‐Philippe Combe A. R. Gillespie

The High Resolution Stereo Camera (HRSC) on the Mars Express (MEx) spacecraft in orbit about Mars is delivering images of the Mars surface and atmosphere from its high‐inclination, elliptical orbit that are intended to cover most of the Mars surface by the end of the mission. These are acquired in four specific spectral passbands that sample the scene at different parts of the extended visual spectrum from near 0.4 μ m to about 1 μ m and in five additional channels, four used for stereo and one nadir, that use the same fifth spectral passband. These channels view from different angles and can be used for photometric and spectral analysis. The data allow a variety of studies of the surface and atmosphere of Mars, but these require detailed understanding of the data characteristics, as there are several effects, including of the observation geometry and the atmosphere, that need to be treated. This article is a report to the science community on the current understanding of the HRSC color data after an initial analysis and also a demonstration of their capabilities for study of Mars, which, from this study, appear to be considerable. We first discuss the characteristics and calibration of the HRSC spectral data. The atmospheric influence on the photometric appearance of the surface materials is explored, and methods of compensating are considered. Reflectances are calculated for surface units by assuming the dark material is basalt and scaling the entire HRSC scene using a laboratory basalt spectrum for the selected dark material area; the results and the correction factors for different orbits are compared. We present several examples of what could become a large volume of future science results utilizing the HRSC spectrophotometric data in conjunction with photo‐interpretation. For example, we find relatively few but very important distinct spectral components at the HRSC resolution, including what we interpret as iron oxide‐rich material, unoxidized basalt, and polar ice, consistent with past works. The major spectral components are distributed in ways that suggest compositional mixing and the need to revise the current geologic understanding of major regions.

Stereo imaging

Spectral resolution

Mars landing

10.1029/2006je002769

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Citations (27)

Tropical to mid-latitude snow and ice accumulation, flow and glaciation on Mars

Nature (2005)

J. W. Head G. Neukum R. Jaumann H. Hiesinger Ernst Hauber

Glacier morphology

Ice core

10.1038/nature03359

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Citations (366)

Phobos control point network, rotation, and shape

Earth and Planetary Science Letters (2009)

Konrad Willner J. Oberst Hauke Hußmann B. Giese H. Hoffmann

Libration (molecule)

Moment of inertia

10.1016/j.epsl.2009.07.033

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Citations (104)

Cloudphysical parameters in dependence on height above cloud base in different clouds

Meteorology and Atmospheric Physics (1989)

H. Hoffmann R. Róth

Liquid water content

Cloud base

Icing conditions

10.1007/bf01026113

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Citations (15)

Dione’s spectral and geological properties

Icarus (2009)

K. Stephan R. Jaumann Roland Wagner R. N. Clark D. P. Cruikshank

Orbiter

10.1016/j.icarus.2009.07.036

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Citations (63)

Evidence for Snow and Ice Accumulation Aiding Debris Flow and Glacial Flow at Mid- to Low-Latitudes on Mars

36th Annual Lunar and Planetary Science Conference (2005)

H. Hiesinger John W. Head G. Neukum R. Jaumann Ernst Hauber

AT MIDTO LOW-LATITUDES ON MARS. H. Hiesinger, J. W. Head, G. Neukum, R. Jaumann, E. Hauber, M. Carr, P. Masson, B. Foing, H. Hoffmann, M. Kreslavsky, S. Werner, S. Milkovich, S. van Gasselt and the HRSC Co-Investigator Team. Dept. Geol. Sci., Brown Univ., Providence RI 02912 USA. Institut fuer Geologische Wissenshaften, Freie Universitaet Berlin, 12249 Berlin, Germany. DLR-Institut fuer Planetenforschung, Berlin, Germany. USGS, Menlo Park CA 94025 USA. Orsay-Terre, Univ. Paris-Sud, Orsay, France. STEC/SCI-ER, Noordwijk, The Netherlands.

Debris flow

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Citations (0)

Geology of the common mouth of the Ares and Tiu Valles, Mars

SoSyR (1998)

A. G. Marchenko A. T. Basilevsky H. Hoffmann Ernst Hauber A. C. Cook

Source

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Citations (13)

A Seasonally Recurrent Annular Cyclone in Mars Northern Latitudes and Observations of a Companion Vortex

Journal of Geophysical Research Planets (2018)

A. Sánchez‐Lavega A. Garro T. del Río‐Gaztelurrutia R. Hueso I. Ordóñez‐Etxeberria

Abstract We study a seasonally recurrent cyclone and related cloud phenomena observed on Mars at L s ~120°, latitude ~60°N, and longitude 90°W from images obtained with cameras in different spacecraft between 1995 and 2018. A remarkable double cyclone formed in 2012 and we present a detailed study of its dynamics using images from Mars Express and Mars Reconnaissance Orbiter obtained between 6 June and 9 July. A double cyclone was also observed in 2006 and 2008. In other Martian years the primary cyclone showed an annular cloud morphology with a large water ice cloud observed eastward of it. The cyclones have a size of ~600–800 km with a cloud‐free core of a radius ~100–300 km. Tangential velocities measured from cloud tracking in 2012 images are ~5–20 m/s −1 at 10‐km altitude and double cyclone moved eastward with a velocity of 4 m/s −1 during its lifetime of one month. The vortices grow in the morning hours, but with the increasing insolation as the sol progresses, a part of the clouds evaporate, the winds weaken, and the vortices lose coherence. This phenomenon forms under high‐temperature gradients in a region with a large north‐south topographic slope and has been recurrent each Martian year between 1995 and 2018. We argue the interest of studying its changing properties each Martian year in order to explore their possible relationship to the state of the Martian atmosphere at L s ~120°.

Atmosphere of Mars

Longitude

Orbiter

10.1029/2018je005740

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Citations (15)

Small-Scale Surface Morphology in the Mouth of Ares and Tiu Valles Region from MOC Images

Lunar and Planetary Science Conference (2000)

Asher Cook A. T. Basilevsky H. Hoffmann G. Neukum

Morphology

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Citations (1)