The Sun is currently a main sequence star and will remain so for another 4-5 billion years. It will then expand and cool to become a red giant, after which it will shrink and heat up again to become a white dwarf. The white dwarf star will run out of nuclear fuel and slowly cool down over many billions of years.
Phosphorus - P - Protons = 15, Electrons = 15, Neutrons = 16 - Non-Metal
Lithium - Li - Protons = 3, Electrons = 3, Neutrons = 4 - Metal
Nitrogen - N - Protons = 7, Electrons = 7, Neutrons = 7 - Non-Metal
Copper - Cu - Protons = 29, Electrons = 29, Neutrons = 34 - Metal
Neon - Ne - Protons = 10, Electrons = 10, Neutrons = 10 - Non-Metal
sorry i don’t know about the other questions but i thought i could help with the table!
Additional Info:
number of protons = atomic number
number of electrons = atomic number
number of neutrons = mass number - atomic number
Since the molecule contains Hydrogen and is covalently bonded, it contains dipole-dipole forces and hydrogen bonds.
Answer:
548 g/mol
Explanation:
The freezing point depression of a solvent occurs when a nonvolatile solute is added to it. Because of the interactions between solute-solvent, it is more difficult to break the bonds, so the phase change will need more energy, and the freezing point will drop, which is called cryoscopy.
The drop in temperature can be calculated by:
ΔT = Kf*W*i
Where Kf is the cryoscopy constant of the solvent, W is the molality, and i is the van't Hoff factor, which indicates the fraction of the solute that dissolves.
The molality represents how much moles (n) of the solute is presented in each kg of the solvent (m2), thus
W = n/m2
The number of moles is the mass of the solute (m1) in g, divided by the molar mass (M1) of it:
W = m1/(M1*m2)
So, by the data:
0.2214 = 0.632/(M1*0.00521)
0.00115M1 = 0.632
M1 = 548 g/mol
