Planned Products of the Mars Structure Service for the InSight Mission to Mars

TLDR: The InSight lander will deliver geophysical instruments to Mars in 2018, including seismometers installed directly on the surface (Seismic Experiment for Interior Structure, SEIS) as discussed by the authors.

Abstract: The InSight lander will deliver geophysical instruments to Mars in 2018, including seismometers installed directly on the surface (Seismic Experiment for Interior Structure, SEIS). Routine operations will be split into two services, the Mars Structure Service (MSS) and Marsquake Service (MQS), which will be responsible, respectively, for defining the structure models and seismicity catalogs from the mission. The MSS will deliver a series of products before the landing, during the operations, and finally to the Planetary Data System (PDS) archive. Prior to the mission, we assembled a suite of a priori models of Mars, based on estimates of bulk composition and thermal profiles. Initial models during the mission will rely on modeling surface waves and impact-generated body waves independent of prior knowledge of structure. Later modeling will include simultaneous inversion of seismic observations for source and structural parameters. We use Bayesian inversion techniques to obtain robust probability distribution functions of interior structure parameters. Shallow structure will be characterized using the hammering of the heatflow probe mole, as well as measurements of surface wave ellipticity. Crustal scale structure will be constrained by measurements of receiver function and broadband Rayleigh wave ellipticity measurements. Core interacting body wave phases should be observable above modeled martian noise levels, allowing us to constrain deep structure. Normal modes of Mars should also be observable and can be used to estimate the globally averaged 1D structure, while combination with results from the InSight radio science mission and orbital observations will allow for constraint of deeper structure.

Figures

Table 1 Major element composition (weight percent) models

Fig. 11 Probability density functions (PDFs) for VS (left) and VP (middle) obtained from a Bayesian inversion of synthetic receiver functions combined with surface wave ellipticity measurements. The right panel shows discontinuity transition expectation, which is the product of the probability of a jump at a given depth with the average shear velocity change of the jump. The input model is shown by the black dashed line, and the mean model from each PDF is shown with a red line

Fig. 12 Ray theoretical spectral ground acceleration amplitude predictions for seismic phases reflected at the core-mantle boundary (PcP, ScS) or transmitted through the core of Mars (PKP, SKS) for a surface source with a seismic moment of 1016 Nm (MW4.6). (a) Seismic velocity profiles for various core sizes based on the bulk composition model of Dreibus and Wänke (1985) (Fig. 1) for the amplitude, travel-time and ray parameter predictions in Figs. 12 and 13. (b) Amplitudes as predicted by ray theory with respect to epicentral distance at frequencies of 0.25 Hz. The minima in PcP amplitude at 25◦ to 30◦ , and 85◦ to 105◦ epicentral distance correspond to a phase shift in the complex reflection coefficient for reflections at the core mantle boundary. (c) Ground acceleration amplitude spectra of PcP, PKP, horizontally polarized ScS and vertically polarized SKS signals for the models in (a) at 60◦ epicentral distance for core-reflected phases PcP and ScS, and at 170◦ epicentral distances for core-transmitted phases PKP and SKS. Black and grey lines mark the mean InSight lander noise (Mimoun et al. 2016, this issue)

Fig. 15 Results of the normal mode inversion. The black dashed lines show the model to retrieve. (a) and (b) show a posteriori probability density functions (PDF) of S wave velocity. Red and blue colors show high and low probabilities, respectively. Continuous black lines represent the minimum and maximum parameter values allowed. Orange curves delimit the interval between ±1σ of the median profile of the distribution. (a) and (b) are the results from the inversion of eigenfrequencies with no noise and including noise, respectively

Fig. 1 A suite of predicted shear wave velocity models for the mantle under Mars conditions for a series of bulk composition models. For each composition, the thick line represents calculated properties for a cold thermal profile, while the thin one represents a hot profile (Plesa et al. 2016). Temperature profiles are shown in Fig. 2. Composition model abbreviations are defined in Table 1. Light blue colored bar represents the L1 and L2 mission requirements for InSight’s ability to resolve elastic structure. The L1–L2 requirements are defined only for the depth region shaded in yellow

Fig. 14 Noise-free (a) and noisy (b) spectra used to compute the eigenfrequencies used in the inversions. Only the peaks with an amplitude larger than a moving RMS (black line) are considered. These are shown in red

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Planned Products of the Mars Structure Service for the
InSight Mission to Mars
M. Panning, Ph. Lognonné, W. Bruce Banerdt, R. Garcia, M. Golombek, S.
Kedar, B. Knapmeyer, A. Mocquet, Nick A. Teanby, J. Tromp, et al.
To cite this version:
M. Panning, Ph. Lognonné, W. Bruce Banerdt, R. Garcia, M. Golombek, et al.. Planned Products of
the Mars Structure Service for the InSight Mission to Mars. Space Science Reviews, Springer Verlag,
2017, 211 (1-4), pp.611-650. �10.1007/s11214-016-0317-5�. �hal-01534998�

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an author's
https://oatao.univ-toulouse.fr/21703
https://doi.org/10.1007/s11214-016-0317-5
Panning, Mark P. and Lognonné, Philippe and Bruce Banerdt, W.,... [et al.] Planned Products of the Mars Structure
Service for the InSight Mission to Mars. (2017) Space Science Reviews, 211 (1-4). 611-650. ISSN 0038-6308

Planned Products of the Mars Structure Service
for the InSight Mission to Mars
Mark P. Panning
1
· Philippe Lognonné
2
· W. Bruce Banerdt
3
· Raphaël Garcia
4
·
Matthew Golombek
3
· Sharon Kedar
3
· Brigitte Knapmeyer-Endrun
5
·
Antoine Mocquet
6
· Nick A. Teanby
7
· Jeroen Tromp
8
· Renee Weber
9
· Eric Beucler
6
·
Jean-Francois Blanchette-Guertin
2
· Ebru Bozdag
˘
10
· Mélanie Drilleau
2
·
Tamara Gudkova
11,12
· Stefanie Hempel
4
· Amir Khan
13
· Vedran Leki
´
c
14
·
Naomi Murdoch
4
· Ana-Catalina Plesa
15
· Atillio Rivoldini
16
· Nicholas Schmerr
14
·
Youyi Ruan
8
· Olivier Verhoeven
6
· Chao Gao
14
· Ulrich Christensen
5
· John Clinton
17
·
Veronique Dehant
16
· Domenico Giardini
13
· David Mimoun
4
· W. Thomas Pike
18
·
Sue Smrekar
3
· Mark Wieczorek
2
· Martin Knapmeyer
15
· James Wookey
7
Abstract The InSight lander will deliver geophysical instruments to Mars in 2018, includ-
ing seismometers installed directly on the surface (Seismic Experiment for Interior Struc-
B
M.P. Panning
mpanning@ufl.edu
1
Department of Geological Sciences, University of Florida, 241 Williamson Hall, Box 112120,
Gainesville, FL 32611, United States
2
Institut de Physique du Globe de Paris, Univ Paris Diderot-Sorbonne Paris Cité,
35 rue Hélène Brion—Case 7071, Lamarck A—75205 Paris Cedex 13, France
3
Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena,
CA 91109, United States
4
Institut Superieur de l’Aeronautique et de l’Espace, Toulouse, France
5
Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen,
Germany
6
Faculté des Sciences et Techniques, Laboratoire de Planétologie et Géodynamique,
UMR-CNRS 6112, Université de Nantes, 2 rue de la Houssinière—BP 92208,
44322 Nantes Cedex 3, France
7
School of Earth Sciences, University of Bristol, Wills Memorial Building, Queens Road,
Bristol BS8 1RJ, United Kingdom
8
Department of Geosciences, Princeton University, Princeton, NJ, United States
9
NASA Marshall Space Flight Center, 320 Sparkman Drive, Huntsville, AL 35805, United States
10
Géoazur, University of Nice Sophia Antipolis, 250 rue Albert Einstein, 06560 Valbonne, France
11
Schmidt Institute of Physics of the Earth, Russian Academy of Sciences, B. Gruzinskaya, 10,
Moscow 123495, Russia
12
Moscow Institute of Physics and Technology (MIPT), Institutsky per., 9, Moscow region, 141700,
Russia

M.P. Panning et al.
ture, SEIS). Routine operations will be split into two services, the Mars Structure Service
(MSS) and Marsquake Service (MQS), which will be responsible, respectively, for defining
the structure models and seismicity catalogs from the mission. The MSS will deliver a series
of products before the landing, during the operations, and finally to the Planetary Data Sys-
tem (PDS) archive. Prior to the mission, we assembled a suite of apriorimodels of Mars,
based on estimates of bulk composition and thermal profiles. Initial models during the mis-
sion will rely on modeling surface waves and impact-generated body waves independent of
prior knowledge of structure. Later modeling will include simultaneous inversion of seismic
observations for source and structural parameters. We use Bayesian inversion techniques
to obtain robust probability distribution functions of interior structure parameters. Shallow
structure will be characterized using the hammering of the heatflow probe mole, as well as
measurements of surface wave ellipticity. Crustal scale structure will be constrained by mea-
surements of receiver function and broadband Rayleigh wave ellipticity measurements. Core
interacting body wave phases should be observable above modeled martian noise levels, al-
lowing us to constrain deep structure. Normal modes of Mars should also be observable and
can be used to estimate the globally averaged 1D structure, while combination with results
from the InSight radio science mission and orbital observations will allow for constraint of
deeper structure.
Keywords Mars · Seismology ·Interior structure · InSight mission
1 Introduction
In order to obtain detailed information on planetary interiors, surface geophysical obser-
vations in general, and seismological measurements in particular are of critical importance
(e.g. Lognonné and Johnson 2007). Much of our knowledge of the internal structure of the
planetary bodies in our solar system is achieved through observations such as gravity field,
rotation, and tides obtained by precisely tracking orbiting spacecraft or landers on the plan-
ets surface, but those observations provide an integrated view of interiors which is generally
non-unique. For the Earth, on the other hand, we have a detailed picture of the interior pri-
marily obtained through the study of seismic data.
Prior to the first recording of global scale seismograms by Von Rebeur-Paschwitz (Von
Rebeur-Paschwitz 1889), the best information on the Earth’s internal structure was deter-
mined from Earth tide analysis (Thomson 1863;Darwin1882). After the advent of quality
seismometers in the late 19th and early 20th centuries, our knowledge of Earth structure ex-
panded rapidly with the discovery of the core by Richard Oldham in 1906, the crust-mantle
discontinuity by Andrija Mohorovi
ˇ
ci
´
c in 1909, and the inner core by Inge Lehmann in 1936.
By 1939, Harold Jeffreys had produced a 1D global model of the whole Earth capable of
matching P wave arrivals within 0.2 % (see e.g. Lay and Wallace 1995, ch. 1). The only other
13
Institut für Geophysik, ETH Zürich, 8092 Zürich, Switzerland
14
Department of Geology, University of Maryland, College Park, MD 20742, United States
15
German Aerospace Center (DLR), Rutherfordstrasse 2, 12489 Berlin, Germany
16
Royal Observatory Belgium, Av Circulaire 3-Ringlaan 3, 1180 Brussels, Belgium
17
Swiss Seismological Service, ETH Zürich, 8092 Zürich, Switzerland
18
Department of Electrical and Electronic Engineering, Imperial College, London, United Kingdom

Planned Products of the Mars Structure Service
planetary body, however, for which we have obtained seismic data unambiguously contain-
ing signals from the interior is the Earth’s moon. The data from seismometers deployed
on the Moon as part of Apollo Passive Seismic Experiment by astronauts in five of the six
Apollo missions between 1969 and 1972, which recorded data until 1977, gave first order
constraints on lunar interior structure, while also producing very unexpected seismograms
showing high levels of scattering (e.g. Nakamura 1983). Perhaps the best illustration of the
power of such scarce planetary seismic data is the number of studies in recent years based
on the Apollo data that have continued to update our understanding of the lunar interior,
including observations of the core and possible deep partial melt, despite not receiving any
new data since the 70’s (Khan and Mosegaard 2002; Lognonné et al. 2003; Chenet et al.
2006; Gagnepain-Beyneix et al. 2006;Khanetal.2007; Weber et al. 2011; Garcia et al.
2011;Zhaoetal.2012; Steinberger et al. 2015; Matsumoto et al. 2015).
The planned InSight lander mission to Mars (Banerdt et al. 2013) will extend planetary
seismology to Mars, and enable other surface geophysical measurements to determine de-
tails of the internal structure and evolution of another terrestrial planet for the first time. The
mission will include 3-component broadband and short period seismometers (Seismic Ex-
periment for Interior Structure, SEIS, Lognonné et al. 2012; Mimoun et al. 2012; Lognonné
and Pike 2015), as well as a heat flow probe (Heat flow and Physical Properties Probe,
HP
3
, Spohn et al. 2014), a geodetic experiment (Rotation and Interior Structure Experiment,
RISE, Folkner et al. 2012), and a magnetometer, in addition to meteorological sensors.
While 2 seismometers were landed on Mars during the Viking missions in the late 1970’s,
the seismometer on Viking 1 did not properly uncage, and the placement of the seismometer
on the top of the Viking 2 lander prevented the recovery of any signals definitively originat-
ing in the planetary interior (Anderson et al. 1977). Twenty years later, a second unsuccess-
ful attempt was made with the OPTIMISM seismometers (Lognonné et al. 1998) onboard
2 Small Autonomous Stations (Linkin et al. 1998) of the failed Mars96 mission. The place-
ment of the sensitive SEIS instrument package directly on the surface of Mars by the InSight
lander, however, is likely to usher in a new era of planetary seismology, enabling broadband
seismology and the recording of seismic and gravimetric signals from tidal frequencies up
to high frequency seismic waves at 50 Hz.
The primary science deliverables from the SEIS instrument are internal structure mod-
els of Mars and a seismicity catalog defining activity on Mars. To that end, the SEIS team
has formed two main services for the mission: the Mars Structure Service (MSS) to focus
on defining the internal structure models and the Marsquake Service (MQS) to catalog the
detected marsquakes and impacts. While the two tasks are intimately related and will re-
quire constant feedback and interaction, these two services provide a structure to ensure the
mission will meet its science goals. In this paper, we describe the major anticipated prod-
ucts of the MSS starting from pre-launch models through initial modeling and refinement
as more data becomes available through the nominal 2 year duration of the mission. This is
meant primarily to serve as a high level overview and summary of the published and ongo-
ing research being done on these topics by researchers within the MSS, and more detailed
descriptions can be found for most techniques and products in the included references. In
the following sections, we detail the products already produced and planned in advance of
the mission (Sect. 2) and anticipated products early in the monitoring phase of the mis-
sion (Sect. 3). We then detail the final anticipated products relating to structure from the
local shallow subsurface (Sect. 4), crust and shallow mantle (Sect. 5), deep mantle and core
(Sect. 6), and planetary scale normal modes and tides (Sect. 7).

Frequently asked questions

Q1. What have the authors contributed in "Planned products of the mars structure service for the insight mission to mars" ?

Panning et al. this paper used the InSight lander to deliver geophysical instruments to Mars in 2018, including seismometers installed directly on the surface. 

Q2. What is the recent workhorse of passive seismic imaging?

Receiver function modeling of P -to-S (Langston 1979) and, more recently, S-to-P (Farra and Vinnik 2000) conversions has been a workhorse of passive seismic imaging of Earth’s crust, mantle lithosphere, and transition zone structure. 

Q3. How many layers are allowed to vary in the mantle?

The number of layers in the mantle is allowed to vary between 2 and 11, with exploration of varying model dimensions accomplished using a type of Bayesian inversion called a transdimensional inversion (e.g. Bodin et al. 2012). 

Q4. What is the way to distinguish between the model families?

A tighter constraint on the maximum regolith thickness, e.g. from analysis of the seismic recordings of HP3 signals or mapping of rocky crater ejecta, would help to distinguish between the model families, and in turn results in tighter constraints on the deeper structure from the ellipticity inversion. 

Q5. How do the authors limit the range of sampled velocities?

The authors limit the range of sampled velocities by setting a minimum VP − VS velocities of 0 km/s (i.e. P wave velocities must be larger than S wave velocities) and a maximum differential of 6 km/s, which is in line with proposed martian seismic velocity models (e.g. Dreibus and Wänke 1985; Sohl and Spohn 1997). 

Q6. What is the method used to estimate the incoming teleseismic and locally converted?

In this method, a free-surface transform can be used to estimate the incoming teleseismic and locally converted wavefields (Kennett 1991) from three component data, and the incoming wavefield is deconvolved from the scattered wavefield to remove source-side complexity and yield a receiver function. 

Q7. Why do the models show more gradual phase transitions in the orthopyroxene?

due to different physical conditions (lower pressure and temperature) and the expected higher iron content of the martian mantle compared to the Earth’s mantle, thermodynamic models constructing the phase equilibria (Khan and Connolly 2008; Rivoldini et al. 2011) show more gradual phase transitions in the orthopyroxene (∼800 km) and the olivine-wadsleyite-ringwoodite-pervoskite system (∼1100 km and ∼1400 km, respectively). 

Q8. How do the authors fit receiver functions together?

The authors start by fitting low-pass filtered versions of the receiver functions (central frequency of 0.1 Hz) together with the ZH ratio data. 

Q9. How can the resolution of core phases on Mars be improved?

The resolution of core phases on Mars can be further improved by applying stacking techniques to account for the expected background noise and interfering seismic phases, especially due to triplications possibly caused by an analog to the Earth’s mantle transition zone at depths between approximately 1000 to 1500 km. 

Q10. What are the common stacking techniques used on Earth?

These stacking techniques are commonly applied on Earth to improve detection of seismic energy of low signal-to-noise ratio (Schweitzer et al. 

Q11. How can the authors recover the firstorder P wave velocity profile?

5.By combining the velocity profiles from the inversion work above, the authors can recover a firstorder P wave velocity profile (shown in Fig. 4c). 

Q12. What are the constraints of the variation of crustal thickness of Mars?

Global scale modeling of gravity and topography variations (e.g. Neumann et al. 2004) give good constraints of the variation of crustal thickness of Mars, but do not constrain the average crustal thickness.