21ST CENT.AST.W/WKBK+SMARTWORK >BI<
6th Edition
ISBN: 9780309341523
Author: Kay
Publisher: NORTON
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Chapter 16, Problem 26QP
To determine
The reason for which a white dwarf move down and to the right along the H-R diagram.
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What is the free-fall time of a 10 MSun main-sequence star?
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The star HD 93250 in the Carina Nebula is a bright O-type star. It has a reported apparent magnitude in the V band of mV = 7.41 and V band absolute magnitude of MV = −6.14.
Using these values calculate the distance to HD 93250 in parsec.
The distance to HD 93250 has been measured by other means as 2350 pc. Compare your calculated value of the distance with the measured value, and give a possible explanation for any difference.
Calculate the value of the interstellar extinction in the V band AV that would account for the difference in the distances.
The parameter E(B − V ) = AB − AV , where AB and AV are the extinctions in the B and V bands, is often used to characterize interstellar extinction. For the star HD 93250 the value E(B − V ) = 0.48 has been measured.
Given the above value of E(B − V ) for HD 93250, calculate the extinction in the B band, and explain why the parameter E(B − V ) is often called the “reddening.”
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Chapter 16 Solutions
21ST CENT.AST.W/WKBK+SMARTWORK >BI<
Ch. 16.1 - Prob. 16.1CYUCh. 16.3 - Prob. 16.3CYUCh. 16.4 - Prob. 16.4CYUCh. 16.5 - Prob. 16.5CYUCh. 16 - Prob. 1QPCh. 16 - Prob. 2QPCh. 16 - Prob. 3QPCh. 16 - Prob. 4QPCh. 16 - Prob. 5QPCh. 16 - Prob. 6QP
Ch. 16 - Prob. 8QPCh. 16 - Prob. 9QPCh. 16 - Prob. 10QPCh. 16 - Prob. 11QPCh. 16 - Prob. 12QPCh. 16 - Prob. 13QPCh. 16 - Prob. 14QPCh. 16 - Prob. 15QPCh. 16 - Prob. 16QPCh. 16 - Prob. 17QPCh. 16 - Prob. 18QPCh. 16 - Prob. 19QPCh. 16 - Prob. 20QPCh. 16 - Prob. 21QPCh. 16 - Prob. 23QPCh. 16 - Prob. 24QPCh. 16 - Prob. 25QPCh. 16 - Prob. 26QPCh. 16 - Prob. 27QPCh. 16 - Prob. 28QPCh. 16 - Prob. 29QPCh. 16 - Prob. 30QPCh. 16 - Prob. 31QPCh. 16 - Prob. 32QPCh. 16 - Prob. 33QPCh. 16 - Prob. 34QPCh. 16 - Prob. 35QPCh. 16 - Prob. 36QPCh. 16 - Prob. 37QPCh. 16 - Prob. 38QPCh. 16 - Prob. 39QPCh. 16 - Prob. 40QPCh. 16 - Prob. 41QPCh. 16 - Prob. 42QPCh. 16 - Prob. 43QPCh. 16 - Prob. 44QPCh. 16 - Prob. 45QP
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- How does a white dwarf differ from a neutron star? How does each form? What keeps each from collapsing under its own weight?arrow_forwardHow much would you weigh if you were suddenly transported to the white dwarf Sirius B? You may use your own weight (or if don’t want to own up to what it is, assume you weigh 70 kg or 150 lb). In this case, assume that the companion to Sirius has a mass equal to that of the Sun and a radius equal to that of Earth. Remember Newton’s law of gravity: F=GM1M2/R2 and that your weight is proportional to the force that you feel. What kind of star should you travel to if you want to lose weight (and not gain it)?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_forward
- If a visual binary system were to have two equal-mass stars, how would they be located relative to the center of the mass of the system? What would you observe as you watched these stars as they orbited the center of mass, assuming very circular orbits, and assuming the orbit was face on to your view?arrow_forwardThe center star in the head of the asterism Scorpius is Dschubba. Assume that Dschubba is a spherical blackbody with a surface temperature of 28,000 K and a radius of 5.16 × 109m, located at a distance of 123 parsecs from Earth. Determine the following for Dschubba:(a) luminosity relative to the Sun (note that L = 3.83 × 1026W ).(b) absolute bolometric magnitude (note that M = 4.74).(c) apparent bolometric magnitude.(d) radiant flux at the star’s surface (in SI unit).(e) radiant flux at Earth’s surface (in SI unit).(f) peak wavelength λmax when plotting the plank function against wavelength (in nm)arrow_forwardHow does the ideal gas law fail in the electron degenerate system of a brown dwarf?arrow_forward
- 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.arrow_forwardA 1.5 M neutron star and a 0.7 M white dwarf have been found orbiting each other with a period of 10 minutes. What is their average separation? Convert your answer to units of the Sun's radius, which is 0.0047 AU.arrow_forwardConsider a white dwarf of mass 1 solar mass and R = 104 km. What is the orbital period of this white dwarf? This represents the minimum possible period that the white dwarf can have; if it rotated any faster, it would break up. How many rotations per second does this correspond to?arrow_forward
- Let's compare the acceleration due to gravity at the surface of a Sun-like star to a white dwarf of similar mass. We know that the force of gravity comes from F= G*m_1*m_2/r^2 and that F = m * a from some of Newton's laws. As such, we know that the acceleration due to gravity is given by a_g = G*m/r^2. With that in mind, let's say that we have a white dwarf star is approximately the size of the Earth which is 1/100 radius of the Sun (0.01 R Sun) and that the white dwarf has a mass that is approximately half the mass of the Sun (0.5 M_Sun). What is the ratio of the acceleration due to gravity at the surface of the white dwarf star (aka the surface gravity) compared to the surface gravity of the Sun-like star (assume its mass is 1 M_sun and radius is 1 R_Sun).?arrow_forwardA visual binary has a parallax of 0.4 arcseconds, a maximum separation a = 6.0 arcseconds, and an orbital period P = 80 years. What is the total mass of the binary system in units of Mo, assuming a circular orbit?arrow_forwardAn O8 V star has an apparent magnitude of +2. Use the method of spectroscopic parallax to estimate the distance to the star. (Hints: the figure below may be helpful.) (answer in parcecs)arrow_forward
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