Foundations of Astronomy (MindTap Course List)
14th Edition
ISBN: 9781337399920
Author: Michael A. Seeds, Dana Backman
Publisher: Cengage Learning
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Chapter 11, Problem 21RQ
To determine
Explain the way in which pressure-temperature thermostat is controlling the nuclear reaction in the interior of star.
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What are the two main nuclear chains known in stars and what are they responsible for? What are the differences between both?
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What is the element that was mostly produced in both processes (PPCR and CNO cycle) and what is the significance to the life cycle of stars?
QUESTION 16
Use the figure shown below to complete the following statement: A low-mass protostar (0.5 to 8M the mass compared to our sun) remains roughly constant in
decreases in
until it makes a turn towards the main sequence, as it follows its evolutionary track.
Protostars of different masses follow diferent
paths on their way to the main sequence.
107
Luminosity (L)
10
105
10
107
10²
101
1
10-1
10-2
10-3
Spectral
type
0.01 R
0.001
Re
60 M
MAIN SEQUENCE
40,000 30,000
20 Mau
10 Mgun
5 Mun
0.1 Run
Ren
radius; temperature
luminosity; radius
3 Min.
05 BO
temperature; luminosity
Oluminosity: temperature
radius: luminosity
1 M
10,000 6000
Surlace temperature (K)
1,000 Rs
2 M STAR
L
0.8 M
B5 AO FOGO КБ МБ
-10
+10
3000
Absolute visual magnitude
and
Chapter 11 Solutions
Foundations of Astronomy (MindTap Course List)
Ch. 11 - Prob. 1RQCh. 11 - Prob. 2RQCh. 11 - Prob. 3RQCh. 11 - Prob. 4RQCh. 11 - During free-fall collapse, what keeps the...Ch. 11 - Prob. 6RQCh. 11 - Prob. 7RQCh. 11 - Prob. 8RQCh. 11 - Prob. 9RQCh. 11 - Prob. 10RQ
Ch. 11 - Prob. 11RQCh. 11 - Prob. 12RQCh. 11 - Prob. 13RQCh. 11 - Describe the three ways thermal energy can be...Ch. 11 - Prob. 15RQCh. 11 - Prob. 16RQCh. 11 - How does the CNO cycle differ from the...Ch. 11 - Prob. 18RQCh. 11 - Prob. 19RQCh. 11 - Prob. 20RQCh. 11 - Prob. 21RQCh. 11 - Prob. 22RQCh. 11 - Prob. 23RQCh. 11 - Prob. 24RQCh. 11 - Prob. 1PCh. 11 - Prob. 2PCh. 11 - Prob. 3PCh. 11 - Prob. 4PCh. 11 - If a protostellar disk is 200 AU in radius and the...Ch. 11 - Prob. 6PCh. 11 - Prob. 7PCh. 11 - Prob. 8PCh. 11 - Prob. 9PCh. 11 - Prob. 10PCh. 11 - Prob. 11PCh. 11 - Prob. 12PCh. 11 - If the Orion Nebula is 8 pc in diameter and has a...Ch. 11 - Prob. 14PCh. 11 - Prob. 1SOPCh. 11 - Prob. 2SOPCh. 11 - Prob. 1LTLCh. 11 - Prob. 2LTLCh. 11 - Prob. 3LTLCh. 11 - Prob. 4LTLCh. 11 - Prob. 5LTLCh. 11 - Prob. 6LTL
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- The text says a star does not change its mass very much during the course of its main-sequence lifetime. While it is on the main sequence, a star converts about 10% of the hydrogen initially present into helium (remember it’s only the core of the star that is hot enough for fusion). Look in earlier chapters to find out what percentage of the hydrogen mass involved in fusion is lost because it is converted to energy. By how much does the mass of the whole star change as a result of fusion? Were we correct to say that the mass of a star does not change significantly while it is on the main sequence?arrow_forwardDo you think that nuclear fusion takes place in the atmospheres of stars? Why or why not?arrow_forwardAccording to the text, a star must be hotter than about 25,000 K to produce an H II region. Both the hottest white dwarfs and main-sequence O stars have temperatures hotter than 25,000 K. Which type of star can ionize more hydrogen? Why?arrow_forward
- Are supergiant stars also extremely massive? Explain the reasoning behind your answer.arrow_forwardH II regions can exist only if there is a nearby star hot enough to ionize hydrogen. Hydrogen is ionized only by radiation with wavelengths shorter than 91.2 nm. What is the temperature of a star that emits its maximum energy at 91.2 nm? (Use Wien’s law from Radiation and Spectra.) Based on this result, what are the spectral types of those stars likely to provide enough energy to produce H II regions?arrow_forwardDescribe the evolution of a star with a mass similar to that of the Sun, from the protostar stage to the time it first becomes a red giant. Give the description in words and then sketch the evolution on an HR diagram.arrow_forward
- If a 100 solar mass star were to have a luminosity of 107 times the Sun’s luminosity, how would such a star’s density compare when it is on the main sequence as an O-type star, and when it is a cool supergiant (M-type)? Use values of temperature from Figure 18.14 or Figure 18.15 and the relationship between luminosity, radius, and temperature as given in Exercise 18.47. Figure 18.15 Schematic HR Diagram for Many Stars. Ninety percent of all stars on such a diagram fall along a narrow band called the main sequence. A minority of stars are found in the upper right; they are both cool (and hence red) and bright, and must be giants. Some stars fall in the lower left of the diagram; they are both hot and dim, and must be white dwarfs. Figure 18.14 HR Diagram for a Selected Sample of Stars. In such diagrams, luminosity is plotted along the vertical axis. Along the horizontal axis, we can plot either temperature or spectral type (also sometimes called spectral class). Several of the brightest stars are identified by name. Most stars fall on the main sequence.arrow_forwardHow do the two types of supernovae discussed in this chapter differ? What kind of star gives rise to each type?arrow_forwardWhat is the heaviest element likely to be produced in fusion processes in stars?arrow_forward
- For a main sequence star with luminosity L, how many kilograms of hydrogen is being converted into helium per second? Use the formula that you derive to estimate the mass of hydrogen atoms that are converted into helium in the interior of the sun (LSun = 3.9 x 1026 W). (Note: the mass of a hydrogen atom is 1 mproton and the mass of a helium atom is 3.97 mproton. You need four hydrogen nuclei to form one helium nucleus.)arrow_forwardPlace the following events in the formation of stars in the proper chronological sequence, with the oldest first and the youngest last. w. the gas and dust in the nebula flatten to a disk shape due to gravity and a steadily increasing rate of angular rotation x. a star emerges when the mass is great enough and the temperature is high enough to trigger thermonuclear fusion in the core y. the rotation of the nebular cloud increases as gas and dust concentrates by gravity within the growing protostar in the center z. some force, perhaps from a nearby supernova, imparts a rotation to a nebular cloud y, then z, then w, then x z, then y, then w, then x w, then y, then z, then x z, then x, then w, then y x, then z, then y, then w MacBook Air on .H. O O O Oarrow_forwardMost stars (Main sequence) generate light through the same mechanism. Because of this, there is an empirical relation between their mass, M, and their Luminosity, L. This relation could be written in the form L/Lsun = (M/Msun, This relation is shown in the log-log diagram below. Find the value of a and round it to the nearest integer. 10 104 102 10-2 10-4 0.1 1.0 2.0 0.2 0.5 5.0 10.0 20.0 Mam (solar masses) Luminosty (solar units)arrow_forward
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