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 16, Problem 57EAP
(a)
To determine
The average number density of particles inside the brown dwarf.
b.
To determine
The temperature required to balance the gas pressure and gravity.
c.
To determine
Whether the estimated temperature can sustain the fusion reaction or not.
d.
To determine
Thechanged conditions inside the brown dwarf.
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Students have asked these similar questions
Convert the average mass density in gm/cm-3 of a M = 0.5 Msun R = 0.015 Rsun white dwarf to the average number density of electrons, ne , in cm-3. Let Z/A = 0.5.
What is the uncertainty in their momentum, Δp, in g-cm/s?
(Hint: you'll need to find the average separation, Δx, between the electrons)
A typical white dwarf has a mass of about 1.0MSunMSun and the radius of Earth (about 6400 kilometers). Calculate the average density of a white dwarf, in kilograms per cubic centimeter.
As a cluster of stars begins to age, which type of star in the cluster will move off the main sequence of the H-R diagram first?
1)
all the stars in a cluster are born at the same time; so they will all move off the main sequence at the same time, as they evolve
2)
G type stars, like our Sun
3)
M type stars, which are the coolest
4)
the lowest mass stars, which have the least amount of fuel for fusion
5)
the O and B type stars
Chapter 16 Solutions
The Cosmic Perspective (9th Edition)
Ch. 16 - Prob. 1VSCCh. 16 - Prob. 2VSCCh. 16 - Prob. 3VSCCh. 16 - Prob. 4VSCCh. 16 - Prob. 1EAPCh. 16 - Prob. 2EAPCh. 16 - Prob. 3EAPCh. 16 - Prob. 4EAPCh. 16 - Prob. 5EAPCh. 16 - Prob. 6EAP
Ch. 16 - Prob. 7EAPCh. 16 - Prob. 8EAPCh. 16 - Prob. 9EAPCh. 16 - Prob. 10EAPCh. 16 - Prob. 11EAPCh. 16 - Prob. 12EAPCh. 16 - Prob. 13EAPCh. 16 - Prob. 14EAPCh. 16 - Prob. 15EAPCh. 16 - Prob. 16EAPCh. 16 - Prob. 17EAPCh. 16 - Prob. 18EAPCh. 16 - Prob. 19EAPCh. 16 - Prob. 20EAPCh. 16 - Prob. 21EAPCh. 16 - Prob. 22EAPCh. 16 - Prob. 23EAPCh. 16 - Prob. 24EAPCh. 16 - Prob. 25EAPCh. 16 - Prob. 26EAPCh. 16 - Prob. 27EAPCh. 16 - Prob. 28EAPCh. 16 - Prob. 29EAPCh. 16 - Prob. 30EAPCh. 16 - Prob. 31EAPCh. 16 - Prob. 32EAPCh. 16 - Prob. 33EAPCh. 16 - Prob. 34EAPCh. 16 - Prob. 35EAPCh. 16 - Prob. 37EAPCh. 16 - Prob. 38EAPCh. 16 - Prob. 39EAPCh. 16 - Prob. 40EAPCh. 16 - Prob. 41EAPCh. 16 - Prob. 42EAPCh. 16 - Prob. 43EAPCh. 16 - Prob. 44EAPCh. 16 - Prob. 45EAPCh. 16 - Prob. 46EAPCh. 16 - Prob. 47EAPCh. 16 - Prob. 48EAPCh. 16 - Prob. 49EAPCh. 16 - Prob. 50EAPCh. 16 - Prob. 51EAPCh. 16 - Prob. 52EAPCh. 16 - Prob. 53EAPCh. 16 - Prob. 54EAPCh. 16 - Prob. 55EAPCh. 16 - Internal Temperature of the Sun. The Sun is...Ch. 16 - Prob. 57EAPCh. 16 - Angular Momentum of a Close Binary. Some close...Ch. 16 - Prob. 59EAP
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- Describe the evolution of a white dwarf over time, in particular how the luminosity, temperature, and radius change.arrow_forwardA supernova can eject material at a velocity of 10,000 km/s. How long would it take a supernova remnant to expand to a radius of 1 AU? How long would it take to expand to a radius of 1 light-years? Assume that the expansion velocity remains constant and use the relationship: expansiontime=distanceexpansionvelocity .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_forward
- Look 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_forwardYou can use the equation in Exercise 22.34 to estimate the approximate ages of the clusters in Figure 22.10, Figure 22.12, and Figure 22.13. Use the information in the figures to determine the luminosity of the most massive star still on the main sequence. Now use the data in Table 18.3 to estimate the mass of this star. Then calculate the age of the cluster. This method is similar to the procedure used by astronomers to obtain the ages of clusters, except that they use actual data and model calculations rather than simply making estimates from a drawing. How do your ages compare with the ages in the text? Figure 22.10 NGC 2264 HR Diagram. Compare this HR diagram to that in Figure 22.8; although the points scatter a bit more here, the theoretical and observational diagrams are remarkably, and satisfyingly, similar. Figure 22.12 Cluster M41. (a) Cluster M41 is older than NGC 2264 (see Figure 22.10) and contains several red giants. Some of its more massive stars are no longer close to the zero-age main sequence (red line). (b) This ground-based photograph shows the open cluster M41. Note that it contains several orange-color stars. These are stars that have exhausted hydrogen in their centers, and have swelled up to become red giants. (credit b: modification of work by NOAO/AURA/NSF) Figure 22.13 HR Diagram for an Older Cluster. We see the HR diagram for a hypothetical older cluster at an age of 4.24 billion years. Note that most of the stars on the upper part of the main sequence have turned off toward the red-giant region. And the most massive stars in the cluster have already died and are no longer on the diagram. Characteristics of Main-Sequence Starsarrow_forwardHow does a white dwarf differ from a neutron star? How does each form? What keeps each from collapsing under its own weight?arrow_forward
- How would the spectra of a type II supernova be different from a type Ia supernova? Hint: Consider the characteristics of the objects that are their source.arrow_forwardWhat is the average density of the white dwarf in Exercise 23.35? How does it compare to the average density of Earth?arrow_forwardThe ring around SN 1987A (Figure 23.12) started interacting with material propelled by the shockwave from the supernova beginning in 1997 (10 years after the explosion). The radius of the ring is approximately 0.75 light-year from the supernova location. How fast is the supernova material moving, assume a constant rate of motion in km/s? Figure 23.12 Ring around Supernova 1987A. These two images show a ring of gas expelled by a red giant star about 30,000 years before the star exploded and was observed as Supernova 1987A. The supernova, which has been artificially dimmed, is located at the center of the ring. The left-hand image was taken in 1997 and the right-hand image in 2003. Note that the number of bright spots has increased from 1 to more than 15 over this time interval. These spots occur where high-speed gas ejected by the supernova and moving at millions of miles per hour has reached the ring and blasted into it. The collision has heated the gas in the ring and caused it to glow more brightly. The fact that we see individual spots suggests that material ejected by the supernova is first hitting narrow, inward-projecting columns of gas in the clumpy ring. The hot spots are the first signs of a dramatic and violent collision between the new and old material that will continue over the next few years. By studying these bright spots, astronomers can determine the composition of the ring and hence learn about the nuclear processes that build heavy elements inside massive stars. (credit: modification of work by NASA, P. Challis, R. Kirshner (Harvard-Smithsonian Center for Astrophysics) and B. Sugerman (STScI))arrow_forward
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