Astronomy- Initial Mass Function problem

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SUMMARY

The discussion focuses on the Initial Mass Function (IMF) in astrophysics, specifically the Salpeter IMF where the exponent α is 2.35. Participants are tasked with deriving an expression for the fraction of stars with mass above a reference mass Mref, using the equations P(m)dm = km−α dm and N(m)dm = NtotP(m)dm. The integration of N(m)dm over the mass range from Mmin (0.07 M) to Mmax (50 M) is essential for normalizing the function. Additionally, the fraction of stars exceeding 8 M is calculated using the derived expressions.

PREREQUISITES
  • Understanding of the Initial Mass Function (IMF)
  • Familiarity with integration techniques in calculus
  • Knowledge of stellar mass ranges (Mmin and Mmax)
  • Basic concepts of probability distribution functions
NEXT STEPS
  • Study the derivation of the Salpeter IMF and its applications in astrophysics
  • Learn integration techniques for probability density functions
  • Explore the implications of stellar mass distributions on galaxy evolution
  • Investigate the relationship between stellar mass and supernova occurrences
USEFUL FOR

Astronomy students, astrophysicists, and researchers interested in stellar formation and mass distribution in star clusters.

StillLearningToronto
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1. Homework Statement

The Initial Mass Function (IMF) defines the distribution of stellar masses created in a star-forming event. The probability P(m)dm of forming a star with a mass between m and m + dm is given by
P(m)dm = km−α dm
where α is the exponent of the power law and k is a constant of proportionality determined by requiring that the probability integrated over all masses be equal to unity. For the Salpeter IMF, which is observed locally,
α = 2.35. If there is a collection of Ntot stars created all at once (e.g., in a cluster or an event in a galaxy), the number N(m)dm of stars with mass between m and m + dm is given by
N(m)dm = NtotP(m)dm
Note that the minimum mass of a star is about m = Mmin = 0.07 M and the maximum mass of a star is about
m = Mmax = 50 M.
SO
a)Symbolically derive an expression for the fraction of the number of stars with a mass above a mass Mref in terms of α, Mref , Mmin, and Mmax. HINT: This will require you to integrate N(m)dm. Make sure to note any conditions you need to impose to carry out the integration.

b)Stars with masses exceeding 8 M explode. Using your result for (b), work out for α = 2.35 the fraction of stars that have a mass above 8 M?

Homework Equations


P(m)dm = km−α dm
N(m)dm = NtotP(m)dm

The Attempt at a Solution


*note i have not taken a proper integration class, which a lot of my issues are coming from, so here's my attempt:
(Mmin//Integral S//Mmax)km^-Alpha dm
k (Mmin//Integral S//Mmax) (m^-alpha+1 dm)/-+1
(k(Mmax)^-alpha+1/-alpha+1) -k(Mmin)^-alpha+1)/-alpha+1
\frac{50^{-α+1}k-0.07^{-α+1}k}/{-α+1}

I know I need to solve for K but I am not sure how to.
After i solve for K for b) I need to somehow put in 8 solar masses, but I am also not sure where that goes into the equation.

Any help is greatly appreciated! Thank you.
 
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StillLearningToronto said:
I know I need to solve for K but I am not sure how to.
Since you're looking for the fraction of stars formed in some range of mass values, it would make sense if you normalized your function over the entire mass range to be unity. Then when you looked at a smaller range, it would give some value between zero and one, i.e. the fraction of the whole.
StillLearningToronto said:
After i solve for K for b) I need to somehow put in 8 solar masses, but I am also not sure where that goes into the equation.
You integrated between mass values of ##M_{min}## and ##M_{max}## to give you the total for the whole possible range. If you plug in other values for those variables, keeping the same value for k, you'll get the fraction of stars between those mass values.
 

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