Linking Core Temperature and Composition With CORE HEAT
We have demonstrated that it is possible to link core temperature and composition during accretion by parameterizing metal/silicate partitioning behavior at high pressure. A key parameter is the average pressure of equilibration for metal and silicate, based on the EOS of liquid metal.
Higher equilibration pressures result in a lower core temperature, because the adiabatic path T (P) of metal is less steep than that of the silicate liquidus.
Product Overview
The BM series features LG’s best efficiency, reducing energy loss in core parts and expanding operation range at low speeds to achieve premium performance. By minimizing resonance and lowering vibration at low-speed, the refrigerator can operate stably. The compressor height is lowered compared to the conventional model, allowing for more space within the refrigerator.
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Features
The BM series features an enlarged core and unique “L” shaped endtanks for improved performance. This allows for better cooling and reduced noise at low speeds. It also enables a much wider operation range for the refrigerator at lower speeds.
The core models are based on bulk compositions of CI or SNC chondrites, the mineralogy of these meteorites (as measured from shock-produced shock casts), and the planetary mass, radius, and moment of inertia that can be computed from their composition. The modelers vary a quasi-adiabatic temperature profile in order to match the planet’s mass, radius, and moment of inertia with core metal, crust, and mantle.
If the inner core is stratified at this temperature, then solid Fe 3-x S 2 will crystallize at its base and snow downward from above, enriching the remaining core liquid in Fe. This will deflect the core liquid’s sulfur content to the adiabat, and will result in an inner core size of about 490 km. This will have a small effect on wavespeeds, changing the ray geometry of SKS and SKKS at the CMB but not significantly altering their form. It will, however, have a large effect on core density, reducing it slightly by about 1%.
Benefits
The results of the experiment showed that core temperature decreases during fluid infusion only if metabolic heat dissipation can keep up. As the core temperature rises, sensible (radiative and convective) and evaporative heat loss mechanisms increase proportionally to the rate of metabolic heating until they equal the rate of thermal cooling, thereby stabilizing the core temperature at the desired value.
The resulting core-to-peripheral temperature gradient and excess core heat thus reflect the degree to which changes in body heat content are disproportionately distributed between the core and peripheral thermal compartments. This constraint of metabolic heat to the core thermal compartment contributes 0.8 +- 0.1 degC and 0.4 +- 0.3 degC, or 30 percent, to the observed core-to-peripheral temperature drop during infusion at 4degC and 20degC fluid, respectively.
If the bulk sulfur content is high enough, core stratification may also suppress dynamo action by increasing the frictional energy required to drive the magnetic field, decreasing Q a d v, and lowering the swarm velocities of tidally driven dynamos (Stewart et al., 2007). Core liquid may then remain at lower temperatures, with solid Fe 3-x CORE HEAT S 2 crystallizing in the center to form iron “snow” that snows downward toward the surface and a composition profile similar to ground fog on Earth. This effect may significantly affect short-range ScP, ScS, and SKKS arrivals.
Applications
When paired with a heart rate monitor, CORE can detect changes in your core body temperature and activate the Intense Endurance Sports Activity algorithm. This algorithm reacts more quickly and accurately to changes in your sporting intensity than the Everyday Living algorithm, which is best suited for low impact activities such as walking, swimming, cycling etc.
The Intense Endurance algorithm also benefits from the addition of 15% more cooling tubes for a greater surface area contact and improved heat dissipation. This reduces the sensitivity to the ambient temperature and increases the accuracy of core body temperature prediction even in cold conditions, when the thermal properties of the skin are less reactive.
At CMB temperatures below 1420 K, solid Fe 3-x S 2 crystallizes at the bottom of the core, enriching it in Fe, and snowing Fe downward from above. This isochoric adiabat has the effect of increasing the inner core radius, if its bulk S content is high enough.
The geochemical/cosmochemical and geophysical models for core formation on Mars used in the analysis differ mainly in the composition of the shallow mantle. The model of Sohl and Spohn (1997) uses a CI chondritic composition for the core, while Rivoldini et al. (2011) use the Dreibus and Wanke (1985) compositional model for their core. Both models yield similar adiabatic temperature profiles, but the ray paths from core-reflected P waves are very different.
