Explanation:
Combustion of a compound is the reaction with oxygen , hence , the process of combustion is an oxidation reaction.
The carbohydrates contain more amount of oxygen as compared to the fats ,
Hence ,
carbohydrates , have a lot of oxygen contents , are are already partially oxidized , but fats have lower oxygen content .
Therefore ,
The partially oxidized carbohydrates are very difficult to oxidized in comparison to fats .
Answer:
its already in scientific notation form however its ordinary or real form is -0.005682
Explanation:
scientific notation
when a number is expressed with some power of 10 multiplied by a number between 1 to 10 is called scientific notation
The change in the standard Gibbs free energy (ΔGº) for the dissociation of nitrous acid (HNO2) at 298 K is 19.09 kJ. If the pH of the solution after equilibrium is reached is 1.30 and the NO2 – concentration at equilibrium is 0.00060 M. What is the equilibrium concentration of HNO2? Hint: Use pH to determine the equilibrium concentration of H+ .
HNO2(aq) H + (aq) + NO2 – (aq)
Answer:
The answer is C. The high solvation energy for LI+
Explanation:
LiF has lower solubility because of the high solvation energy of Li+ ion. This is due to the smaller size and very big charge compared to Cs+ ion which has a bigger size and solvent molecules easily surround it.
Solvation energy is simply the amount energy that is required to make a solute dissolve in a solvent.
B. White Dwarf.
<h3>Explanation</h3>
The star would eventually run out of hydrogen fuel in the core. The core would shrink and heats up. As the temperature in the core increases, some of the helium in the core will undergo the triple-alpha process to produce elements such as Be, C, and O. The triple-alpha process will heat the outer layers of the star and blow them away from the core. This process will take a long time. Meanwhile, a planetary nebula will form.
As the outer layers of gas leave the core and cool down, they become no longer visible. The only thing left is the core of the star. Consider the Chandrasekhar Limit:
Chandrasekhar Limit:
.
A star with core mass smaller than the Chandrasekhar Limit will not overcome electron degeneracy and end up as a white dwarf. Most of the outer layer of the star in question here will be blown away already. The core mass of this star will be only a fraction of its
, which is much smaller than the Chandrasekhar Limit.
As the star completes the triple alpha process, its core continues to get smaller. Eventually, atoms will get so close that electrons from two nearby atoms will almost run into each other. By Pauli Exclusion Principle, that's not going to happen. Electron degeneracy will exert a strong outward force on the core. It would balance the inward gravitational pull and prevent the star from collapsing any further. The star will not go any smaller. Still, it will gain in temperature and glow on the blue end of the spectrum. It will end up as a white dwarf.