The Cosmic Perspective (9th Edition)
9th Edition
ISBN: 9780134874364
Author: Jeffrey O. Bennett, Megan O. Donahue, Nicholas Schneider, Mark Voit
Publisher: PEARSON
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Question
Chapter 17, Problem 48EAP
To determine
The volume of the red giant and the density of the red giant and the density of the red giant compared with the density of the water and with the density of the earth’s atmosphere.
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White Dwarf Size II. The white dwarf, Sirius B, contains 0.98 solar mass, and its density is about 2 x 106 g/cm?. Find the radius of the white dwarf in km to three significant digits. (Hint: Density = mass/volume, and the volume of a
4
sphere is Tr.)
3
km
Compare your answer with the radii of the planets listed in the Table A-10. Which planet is this white dwarf is closely equal to in size?
I Table A-10 I Properties of the Planets
ORBITAL PROPERTIES
Semimajor Axis (a)
Orbital Period (P)
Average Orbital
Velocity (km/s)
Orbital
Inclination
Planet
(AU)
(106 km)
(v)
(days)
Eccentricity
to Ecliptic
Mercury
0.387
57.9
0.241
88.0
47.9
0.206
7.0°
Venus
0.723
108
0.615
224.7
35.0
0.007
3.4°
Earth
1.00
150
1.00
365.3
29.8
0.017
Mars
1.52
228
1.88
687.0
24.1
0.093
1.8°
Jupiter
5.20
779
11.9
4332
13.1
0.049
1.30
Saturn
9.58
1433
29.5
10,759
9.7
0.056
2.5°
30,799
60,190
Uranus
19.23
2877
84.3
6.8
0.044
0.8°
Neptune
* By definition.
30.10
4503
164.8
5.4
0.011
1.8°
PHYSICAL PROPERTIES (Earth = e)…
Place 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 O
Using solar units, we find that a star has 4 times the luminosity of the Sun, a mass 1.25 times the mass of the Sun, and a surface temperature of 4090 K (take the Sun's surface temperature to be 5784 K for the sake of this problem). This means the star has a radius of.................... solar radii and is a .................... star (use the classification).
Chapter 17 Solutions
The Cosmic Perspective (9th Edition)
Ch. 17 - Prob. 1VSCCh. 17 - Prob. 2VSCCh. 17 - Prob. 3VSCCh. 17 - Prob. 4VSCCh. 17 - Prob. 1EAPCh. 17 - Prob. 2EAPCh. 17 - Prob. 3EAPCh. 17 - Prob. 4EAPCh. 17 - Prob. 5EAPCh. 17 - Prob. 6EAP
Ch. 17 - Prob. 7EAPCh. 17 - Prob. 8EAPCh. 17 - What will happen to Earth as the Sun changes in...Ch. 17 - Prob. 10EAPCh. 17 - Prob. 11EAPCh. 17 - Prob. 12EAPCh. 17 - Why cant iron be fused to release energy?Ch. 17 - Prob. 14EAPCh. 17 - Prob. 15EAPCh. 17 - Prob. 16EAPCh. 17 - Does It Make Sense? Decide whether the statement...Ch. 17 - Does It Make Sense? Decide whether the statement...Ch. 17 - Prob. 19EAPCh. 17 - Prob. 20EAPCh. 17 - Prob. 21EAPCh. 17 - Prob. 22EAPCh. 17 - Prob. 23EAPCh. 17 - Prob. 24EAPCh. 17 - Prob. 25EAPCh. 17 - Prob. 26EAPCh. 17 - Prob. 27EAPCh. 17 - Prob. 28EAPCh. 17 - Prob. 29EAPCh. 17 - Prob. 30EAPCh. 17 - Prob. 31EAPCh. 17 - Prob. 32EAPCh. 17 - Prob. 33EAPCh. 17 - Prob. 34EAPCh. 17 - Prob. 35EAPCh. 17 - Prob. 36EAPCh. 17 - Prob. 37EAPCh. 17 - Prob. 39EAPCh. 17 - Prob. 40EAPCh. 17 - Prob. 41EAPCh. 17 - Prob. 42EAPCh. 17 - Prob. 43EAPCh. 17 - Prob. 44EAPCh. 17 - Prob. 47EAPCh. 17 - Prob. 48EAPCh. 17 - Prob. 49EAPCh. 17 - Prob. 50EAPCh. 17 - Prob. 51EAPCh. 17 - Prob. 52EAPCh. 17 - Prob. 53EAPCh. 17 - Prob. 54EAPCh. 17 - The Speed of Supernova Debris. In the year 2001,...
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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
- . The radius of the nebula is about 0.401 light-years. The gas is expanding away from the star at a rate of about 37 kilometers/second . Considering that distance = velocity x time, calculate how long ago the gas left the star if its speed has been constant the whole time. Make sure you use consistent units for time, speed, and distance. Answer in years.arrow_forwardAssuming that at the end of the He burning phase of the stellar core (r < R_core) has no H or He or other metals and is composed completely of Carbon, X=Y=0, X_c = 1 ; The envelope above the core has a normal stellar composition ( r > R_core). Calculate the length of time in years that a 1M_sol and 10M_sol star will live on the horizontal branch or the time between the start and end of the He burning phase. Assume that the normal relationship between mass and luminosity holds for horizontal branch stars. Please be as detailed as possiblearrow_forwardA 46M Sun main sequence star loses 1 Msun of mass over 105 years. (Due to the nature of this problem, do not use rounded intermediate values in your calculations including answers submitted in WebAssign.) How many solar masses did it lose in a year? By how much will its luminosity decrease if this mass loss continues over 0.8 million years? Due to the nature of this problem, for all parts, do not use rounded intermediate values in your calculations-including answers submitted in WebAssign. To determine the number of solar masses lost per year, divide the mass lost by the number of years over which it was lost. Mlost tlost-yr Part 1 of 3 dM = dM = MSun/yrarrow_forward
- A planet orbits 1 AU from a star that is 3.5 times as massive as our Sun. How does the star's luminosity compare? If the star has the same radius as our Sun, what is the temperature of the star compared to the Sun? If Earth's average temperature is 287 K and the Sun were replaced with this star, how would its average temperature change? (Enter a temperature in K. Assume that Earth temperature is proportional to solar flux.)arrow_forwardUse t = 1 M2.5 to compute the life expectancy of a 0.6-solar-mass star. (A solar lifetime is approximately 10 billion years.) yrWhy might this be an underestimate if the star is fully mixed by convection? a) If the star is fully mixed its mass will be much larger than 0.6 solar masses. b) If the star is fully mixed its mass will be much smaller than 0.6 solar masses. c) If the star is fully mixed it will be able to use a larger portion of its hydrogen in fusion than the Sun. d) If the star is fully mixed it will be able to use a smaller portion of its hydrogen in fusion than the Sun.arrow_forwardLook at the four stages shown in Figure 21.8. In which stage(s) can we see the star in visible light? In infrared radiation? Figure 21.8 Formation of a Star. (a) Dense cores form within a molecular cloud. (b) A protostar with a surrounding disk of material forms at the center of a dense core, accumulating additional material from the molecular cloud through gravitational attraction. (c) A stellar wind breaks out but is confined by the disk to flow out along the two poles of the star. (d) Eventually, this wind sweeps away the cloud material and halts the accumulation of additional material, and a newly formed star, surrounded by a disk, becomes observable. These sketches are not drawn to the same scale. The diameter of a typical envelope that is supplying gas to the newly forming star is about 5000 AU. The typical diameter of the disk is about 100 AU or slightly larger than the diameter of the orbit of Pluto.arrow_forward
- Are supergiant stars also extremely massive? Explain the reasoning behind your answer.arrow_forwardIf 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_forward
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