EBK AN INTRODUCTION TO MODERN ASTROPHYS
EBK AN INTRODUCTION TO MODERN ASTROPHYS
2nd Edition
ISBN: 9781108390248
Author: Carroll
Publisher: YUZU
bartleby

Concept explainers

Question
Book Icon
Chapter 8, Problem 8.10P

(a)

To determine

To compare the ratios NII/NI and NIII/NII for the temperatures of 5000K, 15,000K, and 25,000K.

(a)

Expert Solution
Check Mark

Answer to Problem 8.10P

For all the given temperatures, (NII/NI)(NIII/NII).

Explanation of Solution

In the case under consideration, the subscript I stands for neutral helium, II stands for singly ionized helium, and III sands for the completely ionized helium atom.

Given that the ionization energies χI=24.6eV, χII=54.4eV and the partition functions are ZI=1, ZII=2, and ZIII=1. The electron pressure is given as Pe=20Nm2.

Write the expression for the Saha equation in terms of the electron pressure.

  Ni+1Ni=2kTZi+1PeZi(2πmekTh2)3/2eχi/kT        (I)

Here, k is the Boltzmann constant, Pe is the electron pressure, T is the absolute temperature, me is the mass of electron, and h is the Planck’s constant.

Rewrite equation (I) for determining the required ratios.

  NIINI=2kTZIIPeZI(2πmekTh2)3/2eχI/kT        (II)

  NIIINII=2kTZIIIPeZII(2πmekTh2)3/2eχII/kT        (III)

Conclusion:

Substitute 1.38×1023JK1 for k, 5000K for T, 1 for ZI, 2 for ZII, 20Nm2 for Pe, 9.1×1031kg for me, 6.626×1034Js for h, and 24.6eV for χI in equation (II) to find the ratio NII/NI corresponding to temperature 5000K.

NIINI=2(1.38×1023JK1)(5000K)(2)(20Nm2)(1)(2π(9.1×1031kg)(1.38×1023JK1)(5000K)(6.626×1034Js)2)3/2e(24.6eV)(1.38×1023JK1)(5000K)=(1.38 ×1020)(8.518266682 ×1026)e(24.6eV×1.6×1019J1eV)(1.38×1023JK1)(5000K)=1.9×1018

Similarly the values of the ratios NII/NI and NIII/NII can be calculated for different temperatures and the results are tabulated below.

T(K)NII/NINIII/NII
50001.9×10184.3×1049
15,0009.9×1012.4×1011
25,0007.2×1031.8×103

From the table it is clear that the ratio (NII/NI)(NIII/NII) for all the given temperatures.

Therefore, for all the given temperatures, (NII/NI)(NIII/NII).

(b)

To determine

To show that NII/Ntotal=NII(NI+NII+NIII) can be expressed in terms of the ratios NII/NI and NIII/NII.

(b)

Expert Solution
Check Mark

Answer to Problem 8.10P

The ratio NIINtotal=NII(NI+NII+NIII) can be expressed in terms of the ratios NII/NI and NIII/NII as NIINtotal=NII/NI(1+(NII/NI)+(NIII/NII)(NII/NI)).

Explanation of Solution

Given ratio expression is;

  NIINtotal=NII(NI+NII+NIII) (IV)

Take NI as a common factor from the denominator in equation (IV).

  NIINtotal=NIINI(1+NIINI+NIIINI)NIINtotal=(NIINI)(1+NIINI+NIIINI)        (V)

Multiply and divide the third term in the denominator in equation (V) with NII.

  NIINtotal=(NIINI)(1+NIINI+NIIINI×NIINII)NIINtotal=(NIINI)(1+NIINI+(NIIINII)(NIINI))        (VI)

Equation (VI) is the form of the equation (IV) written in terms of the ratios NII/NI and NIII/NII.

Conclusion:

Therefore, the ratio NIINtotal=NII(NI+NII+NIII) can be expressed in terms of the ratios NII/NI and NIII/NII as NIINtotal=NII/NI(1+(NII/NI)+(NIII/NII)(NII/NI)).

(c)

To determine

To plot the graph of NII/Ntotal.

(c)

Expert Solution
Check Mark

Answer to Problem 8.10P

The plot the graph of NII/Ntotal is shown in Figure 1.

Explanation of Solution

The expression for NII/Ntotal written in terms of NII/NI and NIII/NII is given in equation (VI).

  NIINtotal=(NIINI)(1+NIINI+(NIIINII)(NIINI))

From the obtained values of NII/NI and NIII/NII from part (a), the term (NIIINII)(NIINI) can be neglected since they does not contribute significant change to the value of NII/Ntotal for the temperature range 5000K to 25,000K. Thus, equation (VI) becomes;

  NIINtotal=(NIINI)(1+NIINI)        (VII)

With the given values of electron pressure, ionization energies and partition functions for the neutral helium atom and singly ionized helium atom, the ratio NII/NI can be determined for a range of temperatures in between 5000K to 25,000K as shown in part (a). These values can be plugged in to equation (VII) and hence the plot of NII/Ntotal will be obtained.

Conclusion:

The graph of NII/Ntotal is shown in Figure 1 below.

EBK AN INTRODUCTION TO MODERN ASTROPHYS, Chapter 8, Problem 8.10P

From the graph it can be noted that when the temperature corresponding to the partial ionization of the neutral helium is about 15,000K or 1.5×104K.

Want to see more full solutions like this?

Subscribe now to access step-by-step solutions to millions of textbook problems written by subject matter experts!
Students have asked these similar questions
a) b) Electron degeneracy pressure in a white dwarf star, of uniform density p, in the nonrela- tivistic case is given by Pwd ħ² 3memp 25/305/3 where symbols have their usual meanings. Using the result that the central pressure in a star, of radius R and uniform density, under gravitational attraction is given by Pc = Gp² R², derive an expression for the radius Rwd of a white dwarf in terms of its mass M, in the case of nonrelativistic electron degeneracy. Using your result, briefly discuss the limitations of your expression for the radius, in the context of white dwarfs of increasing mass. Consider a white dwarf, mass M, radius Rwd and temperature T, consisting entirely of helium nuclei and electrons. Show that the internal thermal energy of the ions alone is given by 3 M Eth= -kT, 8 mp where mp is the proton mass. White dwarfs initially have a very high temperature when they form, and then cool by radi- ation. Derive a differential equation for the rate of change of the temperature…
The initial stage of star formation is the collapse of a gravitationally unstable volume of gas within a molecular cloud. a Find the Jeans mass and radius for a molecular cloud at a temperature T = 10 K and number density n = 106 cm-3. Assume the mean particle mass is umH, where u = 2.8. Give your answers in solar masses and au, respectively. b Assuming the molecular gas follows the ideal gas law, calculate |dP/dr| = JAP/Ar| ~ Pe/RJ (units [N m-³]) at the beginning of the collapse, where P. is an approximate value for the central pressure of the cloud. Assume that P molecular cloud, and the mass and radius are the values determined above. 0 at the edge of the c Show that |dP/dr| is significantly smaller than GM,p/r². What can you interpret about the core's dynamics from this result?
In a fully degenerate gas, all the particles have energies lower than the Fermi energy.  Using the provided equation for the Fermi energy (EF), and assuming a white dwarf star has a temperature T = 107 K and a mass M = 1Msun, evaluate numerically the ratio Eth/EF, where Eth is the characteristic thermal energy of an electron in a gas of temperature T, to prove that the electrons inside a white dwarf are indeed degenerate. (Hint: Estimate the characteristic density (ne) based on the given conditions inside a white dwarf)
Knowledge Booster
Background pattern image
Physics
Learn more about
Need a deep-dive on the concept behind this application? Look no further. Learn more about this topic, physics and related others by exploring similar questions and additional content below.
Similar questions
SEE MORE QUESTIONS
Recommended textbooks for you
Text book image
College Physics
Physics
ISBN:9781305952300
Author:Raymond A. Serway, Chris Vuille
Publisher:Cengage Learning
Text book image
University Physics (14th Edition)
Physics
ISBN:9780133969290
Author:Hugh D. Young, Roger A. Freedman
Publisher:PEARSON
Text book image
Introduction To Quantum Mechanics
Physics
ISBN:9781107189638
Author:Griffiths, David J., Schroeter, Darrell F.
Publisher:Cambridge University Press
Text book image
Physics for Scientists and Engineers
Physics
ISBN:9781337553278
Author:Raymond A. Serway, John W. Jewett
Publisher:Cengage Learning
Text book image
Lecture- Tutorials for Introductory Astronomy
Physics
ISBN:9780321820464
Author:Edward E. Prather, Tim P. Slater, Jeff P. Adams, Gina Brissenden
Publisher:Addison-Wesley
Text book image
College Physics: A Strategic Approach (4th Editio...
Physics
ISBN:9780134609034
Author:Randall D. Knight (Professor Emeritus), Brian Jones, Stuart Field
Publisher:PEARSON