Universe: Stars And Galaxies
6th Edition
ISBN: 9781319115098
Author: Roger Freedman, Robert Geller, William J. Kaufmann
Publisher: W. H. Freeman
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Question
Chapter 20, Problem 33Q
To determine
Better names for brown dwarfs, red dwarfs and white dwarfs and the way these alternative names describe the objects’ properties accurately.
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Students have asked these similar questions
Which of the following is least reasonable regarding the mass of stars?
Group of answer choices
The vast majority of stars fall into the range of 0.08 to 100 solar mass.
Stars which are too small cannot sustain nuclear fusion.
Stars which are excessively big are too sluggish to sustain nuclear fusion.
There are more stars on the low end than on the high end of the mass spectrum.
A brown dwarf has a mass just below the least massive star.
Use the H-R Diagram below to help answer the following
questions.
Luminosity (solar units)
10,000+
1,000+
100+
10-
.01+
.001+
.0001
B
White Dwarfs
20,000
B
Spectral Type
A
Main
Sequence
D
10,000
Temperature (K)
FGK
Red Giants
5,000
M
-5
10
15
Absolute Magnitude
Globular clusters contain no stars more massive than the Sun. Which of the following seems like the least reasonable implication of this observation?
Group of answer choices
Globular clusters are very old.
Globular clusters are very young.
Only the low-mass stars are still "alive" in the clusters.
Many red giants can probably be found in globular clusters.
The very massive stars in the globular clusters have already burnt out.
Chapter 20 Solutions
Universe: Stars And Galaxies
Ch. 20 - Prob. 1QCh. 20 - Prob. 2QCh. 20 - Prob. 3QCh. 20 - Prob. 4QCh. 20 - Prob. 5QCh. 20 - Prob. 6QCh. 20 - Prob. 7QCh. 20 - Prob. 8QCh. 20 - Prob. 9QCh. 20 - Prob. 10Q
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- How do we distinguish stars from brown dwarfs? How do we distinguish brown dwarfs from planets?arrow_forwardConsider the following five kinds of objects: open cluster, giant molecular cloud, globular cluster, group of O and B stars, and planetary nebulae. A. Which occur only in spiral arms? B. Which occur only in the parts of the Galaxy other than the spiral arms? C. Which are thought to be very young? D. Which are thought to be very old? E. Which have the hottest stars?arrow_forwardLook elsewhere in this book for necessary data, and indicate what the final stage of evolution-white dwarf, neutron star, or black hole-will be for each of these kinds of stars. A. Spectral type-O main-sequence star B. Spectral type-B main-sequence star C. Spectral type-A main-sequence star D. Spectral type-G main-sequence star E. Spectral type-M main-sequence stararrow_forward
- Describe several characteristics that distinguish population I stars from population II stars.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_forwardMatch the spectral type and luminosity class to theletters shown on the Hertzsprung-Russell diagram 1) A WD (White Dwarf)2) G V (Main Sequence) 3) M V (Main Sequence)4) M I (Supergiant)5) G III (Giant)arrow_forward
- Which of the following is least reasonable regarding novae and supernovae? Group of answer choices A type I (carbon-detonation) supernova results when a white dwarf in a binary system absorbs enough mass from its companion to push it over the Chandrasekhar limit. A type II supernova results from any supermassive star at the end of its life, when it runs out of fusion energy and collapses. A nova can occur multiple times in a binary system. If a white dwarf in a binary system absorbs enough mass to go beyond the Chandrasekhar limit, the white dwarf explodes as a supernova. The reason a type I supernova does not produce hydrogen lines is that the explosion originates from a stellar core (white dwarf), where hydrogen has already fused to produce heavier elements (so there is no longer any hydrogen). More supernovae are observed in the Milky Way because they are much closer to us than those in other galaxies.arrow_forwardList the following 5 terms in order through a stars life cycle (starting with the sun), through the remainder of its lifetime: a. Black dwarf b. Planetary nebula c. Red giant d. Star (Sun) e. White dwarfarrow_forwardWhich of the following most correctly explains why we have not yet observed any white dwarfs derived from M stars: Group of answer choices Most M stars end up as neutron stars or black holes. The lifetime of M stars is longer than the age of the universe. Most M stars are located near the edge of the universe, beyond the visible horizon. Most M stars are members of a binary system, and the white dwarf would be obscured by the glare of the more massive companion. White dwarfs are too dim to be observed with currently available techniques.arrow_forward
- The sketch below shows an H-R diagram for a star cluster. Consider the star to which the arrow points. How is it currently generating energy? Temperature A. by hydrogen shell burning around an inert helium core B. by gravitational contraction C. by core hydrogen fusion D.by core helium fusion combined with hydrogen shell burning E. by both hydrogen and helium shell burning around an inert carbon core Luminosity -→arrow_forwardLet’s say you’re looking for extrasolar planets. You observe a star that has a spectral shift in the line that is supposed to be at at 656.28011 nm – this star shows this line at 656.28005 nm. What is the radial velocity of star (in m/s) and in what direction in relation to you? a) 27.4 m/s, towards b) 27.4 km/s, away c) -27.4 m/s, toward d) -27.4 km/s, awayarrow_forwardQUESTION 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 andarrow_forward
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