What is the Mass-Radius Relation for a White Dwarf with 0.6 Solar Masses?

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SUMMARY

The discussion focuses on calculating the radius of a white dwarf with a mass of 0.6 solar masses, utilizing the mass-radius relation and properties of an electron gas. The numerical constant C was determined to be 31.57 using Avogadro's number (N0 = 6.02 x 10^23) and relevant equations. The final computed radius was found to be approximately 107.98 meters, prompting a review of unit conversions and density parameters to ensure accuracy. The importance of consistent unit usage in calculations was emphasized to avoid errors in astrophysical computations.

PREREQUISITES
  • Understanding of the mass-radius relation for white dwarfs
  • Familiarity with the properties of electron gases
  • Knowledge of Avogadro's number and its application in calculations
  • Proficiency in unit conversions, particularly between grams, kilograms, and cubic meters
NEXT STEPS
  • Research the mass-radius relation for different types of stellar remnants
  • Learn about the role of electron degeneracy pressure in white dwarfs
  • Explore advanced unit conversion techniques in astrophysics
  • Investigate the implications of density variations in stellar structures
USEFUL FOR

Astronomy students, astrophysicists, and anyone interested in stellar evolution and the properties of white dwarfs will benefit from this discussion.

Catria
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Homework Statement



Compute the numerical constant C for an electron gas (take Z = 6 and A = 12) and determine the radius of a white dwarf whose mass is 0.6 solar masses.

h\ =\ 6.62606876(52)\ \times\ 10^{-34}\ Jh\ =\ 6.62606876(52)\ \times\ 10^{-34}\ J\ s\ s

m_{e}\ =\ 9.10938188(72)\ \times\ 10^{-31}\ kg

G\ =\ 6.673(10)\ \times\ 10^{-11}G\ =\ 6.673(10)\ \times\ 10^{-11}\ m^{3} kg^{-1} s^{-2}\ m^{3} kg^{-1} s^{-2}

Mass of the white dwarf: \ 1.2 \times\ 10^{30}kg

Homework Equations



M = \frac{f}{R^{3}}

f = \frac{π}{3}\left(\frac{15C}{2πG} \right)^{3}

\frac{N}{V} = \frac{ρN_{0}}{2}, since Z/A = 1/2

P=Cρ^{\frac{5}{3}} = \left(\frac{N}{V}\right)^{\frac{5}{3}} \left(\frac{3h^{3}}{8π}\right)^{\frac{2}{3}}\frac{1}{5m}

The Attempt at a Solution



C = \frac{1.064\times10^{-67}}{5m}\left(\frac{N_{0}}{2}\right)^{\frac{5}{3}}

I took N_{0} = 6.02 x 10^{23} so C = 31.57

\frac{15C}{2πG}=\frac{473.53}{4.19\times 10^{-10}}=1.13\times10^{12}

Putting that into f, we get f = 1.511\times10^{36}

Now, 1.2\times10^{30} = \frac{1.511\times10^{36}}{R^{3}}

and finally R = 107.98m, which doesn't make any sense to me. The only place where I think I might have it wrong is the value of N_{0}.
 
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Working with units would help to spot the error.
What is N0? If it is the avogadro constant, why do you get it as factor between a density and another density? Which units do you use for ρ?
 
I hate the textbook and the class notes but, per class notes, I assume ρ is in g/cc, and N/V is in particles per cubic meter.
 
cc? cm3? Then you need an additional factor of 10^6 to convert between m3 and cm3.
 
But then I'd have to divide by 1,000 to go from grams to kilograms... so I'd need an additional factor of 1,000 rather than 10^6.
 
As you can see, it would be useful to work with units everywhere. It is easier to spot (or avoid) those prefactors if you know the units of your parameters.
 
And now it gives a more sensible size (somewhat larger than Earth in volume, yet on the same order of magnitude); I find that the Coulomb pressure wouldn't affect the radius very much.
 

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