visual
前期参数文件准备
- 打开
movie_subface和movie_volume并保持movie_coarse关闭
GMT 画图
- 命令行输入：
1
./bin/xcreate_movie_AVS_DX
该命令会使 moviedata*** 转换为可读文件 gmt_movie_***.Z.xyz
其实 `gmt_movie**.pl` 是生成一个 `plot_movie.csh` 文件，主要是使用 gmt 命令, 如：xyps, xyz2grd,
ps2pdf
install
1 | brew install ghostscript |
Model
Par_file
各个模型
1D models with real structure:
1D_isotropic_prem Isotropic version of the spherically symmetric Preliminary Reference Earth Model (PREM) [Dziewo ́ nski and Anderson, 1981].
1D_transversely_isotropic_prem Transversely isotropic version of PREM.
1D_iasp91 Spherically symmetric isotropic IASP91 model [Kennett and Engdahl, 1991].
1D_1066a Spherically symmetric earth model 1066A [Gilbert and Dziewo ́ nski, 1975]. When ATTENTUATION is on, it uses an unpublished 1D attenuation model from Scripps.
1D_ak135f_no_mud Spherically symmetric isotropic AK135 model [Kennett et al., 1995] modified to use the density and Q attenuation models of Montagner and Kennett [1995]. That modified model is traditionally called AK135-F, see http://rses.anu.edu.au/seismology/ak135/ak135f.html for more details. As we do not want to use the 300 m-thick mud layer from that model nor the ocean layer, above the d120 discontinuity we switch back to the classical AK135 model of Kennett et al. [1995], i.e., we use AK135-F below and AK135 above.
1D_ref A 1D Earth model developed by Kustowski et al. [2006]. This model is the 1D background model for the 3D models s362ani, s362wmani, s362ani_prem, and s29ea.
1D_CCREM A 1D Earth model developed by Ma and Tkalcic [2021] called CCREM: a new reference Earth model from the global coda-correlation wavefield. Ishii Combines the 1D transversely isotropic PREM with the anisotropic inner core model defined by Ishii et al. [2002].
for Mars:
1D_Sohl 1D Mars model developed by Sohl and Spohn [1997]. This model is model A, mostly constrained by geophysical moment of inertia.
1D_case65TAY 1D Mars reference model developed by Plesa et al. [2021]. The model is the 1D reference model for case 65 with a compositional model by Taylor.
mars_1D 1D Mars model as defined in file mars_1D.dat in folder DATA/mars.
for Moon:
VPREMOON 1D Moon model developed by Garcia et al. [2011]. Uses modified seismic model, starting from table 6 (left side, not geodesic model) with velocity values for outer core and solid inner core based on Weber et al. [2011]
Fully 3D models:
transversely_isotropic_prem_plus_3D_crust_2.0 This model has CRUST2.0 [Bassin et al., 2000] on top of a transversely isotropic PREM. We first extrapolate PREM mantle velocity up to the surface, then overwrite the model with CRUST2.0
s20rts By default, the code uses 3D mantle model S20RTS [Ritsema et al., 1999] and 3D crustal model Crust2.0 [Bassin et al., 2000]. Note that S20RTS uses transversely isotropic PREM as a background model, and that we use the PREM radial attenuation model when ATTENUATION is incorporated. See Chapter 12 for a discussion on how to change 3D models.
s40rts A global 3D mantle model [Ritsema et al., 2011] succeeding S20RTS with a higher resolution. S40RTS uses transversely isotropic PREM as a backgroun model and the 3D crustal model Crust2.0 [Bassin et al., 2000]. We use the PREM radial attenuation model when ATTENUATION is incorporated.
s362ani A global shear-wave speed model developed by Kustowski et al. [2006]. In this model, radial anisotropy is confined to the uppermost mantle. The model (and the corresponding mesh) incorporate tomography on the 650 km and 410 km discontinuities in the 1D reference model REF.
s362wmani A version of S362ANI with anisotropy allowed throughout the mantle.
s362ani_prem A version of S362ANI calculated using PREM as the 1D reference model.
s29ea A global model with higher resolution in the upper mantle beneath Eurasia calculated using REF as the 1D reference model
3D_anisotropic See Chapter 12 for a discussion on how to specify your own 3D anisotropic model.
3D_attenuation See Chapter 12 for a discussion on how to specify your own 3D attenuation model.
PPM For a user-specified 3D model (Point-Profile-Model) given as ASCII-table, specifying Vs-perturbations with respect to PREM. See Chapter 12 for a discussion on how to specify your own 3D model.
full_sh For a user-specified, transversely isotropic 3D model given in spherical harmonics. Coefficients for the crustal model (up to degree 40) are stored in files named C**.dat and MOHO.dat, coefficients for the mantle model (up to degree 20) are stored in files named M**.dat. All model files reside in directory DATA/full_sphericalharmonic_model/. Note that to use the crustal model, one has to set the crustal type value ITYPE_CRUSTAL_MODEL = ICRUST_CRUST_SH in file setup/constants.h. This crustal model can be transversely isotropic as well.
sgloberani_iso By default, the code uses 3D isotropic mantle model SGLOBE-rani [Chang et al., 2015] and the 3D crustal model includes perturbations from Crust2.0 [Bassin et al., 2000] as discussed in [Chang et al., 2015]. The model is parametrised horizontally in spherical harmonics up to lmax=35 and with 21 depth splines for the radial direction. Note that SGLOBE-rani uses transversely isotropic PREM as a background model, and that we use the PREM radial attenuation model when ATTENUATION is incorporated.
sgloberani_aniso By default, the code uses 3D anisotropic mantle model SGLOBE-rani [Chang et al., 2015] and the 3D crustal model includes perturbations from Crust2.0 [Bassin et al., 2000] as discussed in [Chang et al., 2015]. Note that SGLOBE-rani uses transversely isotropic PREM as a background model, and that we use the PREM radial attenuation model when ATTENUATION is incorporated.
sgloberani_aniso By default, the code uses 3D anisotropic mantle model SGLOBE-rani [Chang et al., 2015] and the 3D crustal model includes perturbations from Crust2.0 [Bassin et al., 2000] as discussed in [Chang et al., 2015]. Note that SGLOBE-rani uses transversely isotropic PREM as a background model, and that we use the PREM radial attenuation model when ATTENUATION is incorporated.
SPiRaL A multiresolution global tomography model of seismic wave speeds and radial anisotropy variations in the crust and mantle developed by Simmons et al. [2021]. Please see folder DATA/spiral1.4 for further information on how to install the corresponding model files.
GLAD_bkmns A Block Mantle & Spherical Harmonics (BKMNS) expansion model developed by Ciardelli et al. [submitted.] for global crust/mantle 3D models GLAD-M25 and GLAD-M15. Please see folder DATA/gladm25 for further information on how to install the corresponding model files.
for Mars:
1D_Sohl_3d_crust This model adds a 3D crust on top of the 1D Mars model developed by Sohl and Spohn [1997]. The crustal model is defined by the files in folder DATA/crustmaps/marscrust*.cmap
1D_case65TAY_3d_crust This model adds a 3D crust on top of the 1D Mars model developed by Plesa et al. [2021]. The crustal model is defined by the files in folder DATA/crustmaps/marscrust*.cmap
