- #1
jk4
The book gives the equation:
[tex]\frac{\Delta\textit{v}}{\textit{v}} = \frac{GM}{c^{2}R}[/tex]
the problem gives me the mass of the sun, it's radius, and the wavelength of light being emitted.
So basically I can solve the right side of the equation, but I'm just not sure about how to express the amount of "red shift". Is it the entire left side? or is it just the top of the fraction on the left side? Or something else. I've tried both and don't get the books answer.
According to the book:
Sun mass = 2.0x10^(30) kg
Sun radius = 7.0x10^(8) m
wavelength of light = 500 nm (being emitted by the sun)
"Find the approximate gravitational red shift"
The book answer is 1.06 pm
[EDIT]
I'll throw this in too. the constant G = 6.673x10^(-11) N m^(2) / kg^(2)
[tex]\frac{\Delta\textit{v}}{\textit{v}} = \frac{GM}{c^{2}R}[/tex]
the problem gives me the mass of the sun, it's radius, and the wavelength of light being emitted.
So basically I can solve the right side of the equation, but I'm just not sure about how to express the amount of "red shift". Is it the entire left side? or is it just the top of the fraction on the left side? Or something else. I've tried both and don't get the books answer.
According to the book:
Sun mass = 2.0x10^(30) kg
Sun radius = 7.0x10^(8) m
wavelength of light = 500 nm (being emitted by the sun)
"Find the approximate gravitational red shift"
The book answer is 1.06 pm
[EDIT]
I'll throw this in too. the constant G = 6.673x10^(-11) N m^(2) / kg^(2)