User:Kzhan15/sandbox

Basic concept and value
This article talks about the differences in volcanic mechanisms between Earth and Mars and major volcanoes on Mars.

Alteration to the content
It's true that there are many typical volcanoes on Mars. However, the author should list only Top3 volcanoes of them and save the space talking about how volcanism was involved in the geological evolution on Mars.

Coments on words part
Successful part: The best part of it is to compare volcanism and other geological features with Earth. Some are quite similar while others are different. It is easy for those characteristics to evoke our curious and keep asking why they have those similarities and differences? This may lead to more people get interested in Mars and do a further research.

Improve-able part: There shouldn't be so many volcanic provinces talked about in the article.

Coments on figure part
Successful part: Figures "Schematic diagrams showing the principles behind fractional crystallisation in a magma" and "Planet Mars - volatile gases"are very simple, clear and easy for audience to remember. Improve-able part: The "X-ray"Figure is quite confusing. I think it needs some more explanations of how the figure is related to the conclusion.Because there are just rings and audience may not know what does the ring and their sequences mean.

Basic concept and value
It describes characteristics of the surface features of Mars: slope streaks, dust devil tracks, sand dunes, Medusae Fossae Formation, fretted terrain, and Chaos terrain and contains reasons why some features are formed.

Alteration to the content
These features should be divided into different parts due to the cause of formations. The classifies could be formed by water, wind or unknown forces.

Comments on words part
Successful part:This article talks about the characteristics, causes(if known),locations of each features which give audience a whole view of them.

Improve-able part: Since the Slope streaks have been discovered recently, more and more information can be added to this article in the future such as the cause, and growing rate.

Coments on figure part
Successful part: At least 3 pictures are listed under each feature. Because they are taken by HiRISE， this is the best way to show us what each feature is really like on a planet that we can't set foot on.

Improve-able part: Medusae Fossae Formation is a deposit that along the equator of Mars. It could be better if pictures taken from a little bit above the equator that show the position and Medusae Fossae Formation are attached.

Basic concept and value
This article talks about the evidence for existence of groundwater on Mars: Layered terrain and Inverted terrain, and evidence for groundwater upwelling.

Alteration to the content
There are new evidence of groundwater-fed lake on Mars recently found by NASA's Mars Reconnaissance Orbiter. This should be added to the content.

Comments on words part
Successful part: At the end of first part, it points out the same process has happened on Earth. It shows another similarity between Mars and Earth.

Improve-able part: Since this mainly focus groundwater, the second paragraph which indicates terrain inversion can also happen by wind could be omitted.

Comments on figure part
Successful part: Figure under "Layered terrain" part is useful, it makes the process of groundwater helps form layers straightforward.

Improve-able part: In "Layered terrain" part, it says "layers in intercrater regions have been observed". So, if there is a picture posted with it should be perfect.

Content
(!)Introduction, (2)Kinematic models involving narrow gradens,(3)Stress

Content
(!)Introduction,(2)Geography and Constraints, (3) Process at mid-ocean ridge.

Values to audiences and geologiests for both topics
It gives them an overview of the structural history of that region Through reading, geologists could exchange notions and edit more to it and make it complete.

Figures
The original figures will not be so complicated and will forcus on the process of evolution or models which intends to make it easier for audience to understand.

Geodynamics on Mars
The past years have been particularly fruitful for Martian research as the enormous volumes of data collected during the Viking mission became readily available to the general science community, and as reformatting of the remote sensing data into cartographic products made the data more usable. Other than Martian structures on the surface, geodynamic problems also draw scientists’ interests. A lot of theories about Martian core, mantle, and crust have been addressed, because it provides a better understanding of seeable tectonics, mountains and internal activity..

Introduction
The upper and lower bound on the initial mantle temperature are 2450K and 1600K [Zhang, J., and C. Herzberg (1994), Melting experiments on anhydrous peridotite KLB-1 from 5.0 to 22.5 GPa]. According to Elkins-Tanton et al.’s calculations, the core-mantle temperature contrast due to mantle overturn is on the order of ~1000K [ET2005]. As a result, it seems very likely that the mantle was substantially molten and a completely or partially molten layer (TBL-thermal boundary layer) formed at the base of the mantle [coupled core-mantle evolution].

Model and results
In Y. Ke1 and V. S. Solomatov’s model, the core is liquid and is vigorously convecting [coupled core-mantle]. The heat flxu out of the TBL (at the upper boundary) is close to zero because the temperature profile above the TBL quickly reaches a steady state profile in the frame of reference associated with the moving upper boundary of the TBL[ Solomatov and Moresi 2002]. As the core temperature decreases, the driving temperature difference for convection inside the TBL decreases, and the heat flxu decreases[coupled]. Cooling and crystallization of the molten TBL is very fast(~100 years). After the melt fraction drops to ~40% the viscosity significantly increases and the CMB temperature continues to decrease at a much slower rate[coupled]. When a relatively modest viscosity contrast between the TBL ( at the rheological transition) and the mantle is achieved, a superplume is generated [ Ke and Solomatov 2006]. According to their model, the coupled core-mantle thermal evolution can be divided into three stages: (1) the growth of the internally convecting thermal boundary layer, (2) the superplume formation, and (3) the spread and decay of the superplume[coupled].

Introduction
The coupled evolution of the mantle and crust is one of the most significant problems in the geodynamics of terrestrial planets [Lenardic and Moresi 1999]. Mars is a one-plate planet, and likely has been for much, if not all, of its history [Thermal and crustal]. In one-plate planet, heat is generated by radioactive decay and transported to the surface by heat conduction through a single plate lying on top of a convecting mantle which is stagnant lid convection .[Early plate tectonics versus single]. Stagnant lid convection can occur in two regimes: steady and time-dependent.

Model and results
In Steven A. Hauck II1 and Roger J. Phillips’ model, calculations are for time-dependent convection. The model covers the time period from 4.5Ga to the present. According to their model, total crustal thickness is ~62km, and the fractional crustal growth (fraction of maximum crust generated within the simulation) at 4 Ga is ~73. Pervasive partial melting ends by ~2.8 Ga. Extraction of heat from the core is relatively small throughout most of the simulation, but the heat flux out of the core in Figure 2c may be quite significant during the first few hundred million years. The early growth in surface heat flux is due to cooling of new crust and the presence of heat-produing elements in that crust. The relative fraction of the total heat production that is generated in the crust is illustrated in Figure 2e with a total amount equal ~26% of all heat production. Average and maximum volume melt fractions as a function of time are shown in Figure 2f. The bulk crust represents an average melt fraction of ~10%.