EBK PHYSICS FOR SCIENTISTS & ENGINEERS
5th Edition
ISBN: 9780134296074
Author: GIANCOLI
Publisher: VST
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Chapter 44, Problem 51GP
To determine
The ratio of the diameter of the two stars that have spectra peaks at
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An astronomical image shows two objects that have the same apparent magnitude, i.e., the same brightness. However, spectroscopic follow up observations indicate that while one is a star that is within our galaxy, at a distance dgal away, and has the same luminosity as the Sun, the other is a quasar and has 100x the luminosity of the entire Milky Way galaxy. What is the distance to the quasar? (You may assume, for this rough calculation, that the Milky Way has 1011 stars and that they all have the luminosity as the Sun.) Give your response in Mpc. Value: dgal = 49 pc
B9
Assuming stars to behave as black bodies stefan-boltzmann law to show that the luminosity of a star is related to its surface temperature and size in the following way:
L = 4(3.14)R^2oT^4
where o= 5.67 ×10^-8 Wm^-2 K-4 is the stefan- boltzmann constant. Then use this expression together with the knowledge that the sun has a surface temperature of 5700k and radius 695 500km to calculate the luminosity of the Sun in units of Watts
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- From the light and velocity curves of an eclipsing spectroscopic binary star system, it is determined that the orbital period is 6.31 yr and the maximum radial velocities of stars A and B are 5.4 km/s and 22.4 km/s, respectively. Furthermore, the time period between first contact and minimum light (tp-ta) is 0.58 d and the length of the primary minimum (tc-tb) is 0.64 d. From this information, assuming circular orbits, find: a) the ratio of stellar masses. b) the sum of masses (i ~ 90°). c) the individual masses. d) the individual radii.arrow_forwardQuestion 2: apparent magnitude my 1 = 305.9, b = −44.9 and is d=4.5 kpc from the Sun. a.) The integrated light from the Milky Way globular cluster NGC 104 has an 4.03 mag and absolute magnitude My -9.52 mag. It is located at b.) = = Estimate the amount of extinction between the Sun and 47 Tucanae in magnitudes. What does this value of extinction mean for the amount of attenuation by dust between Earth and NGC 104?.arrow_forwardFor the PP chain 0.7% of the mass participating in nuclear fusion is liberated as energy which produces a star's luminosity. Assume that the core of a main sequence star consists of 10% of its total mass. Hence, estimate the lifetime of a star on the main sequence in terms of its luminosity L/L. Give your answer in years. You may use the observed mass-luminosity relation L x M³.5, where M is the star's total mass. Using typical values, calculate estimates for the main sequence lifetime of a KO star and a 05 star. Describe briefly why your estimate might be more accurate for K stars compared to O stars.arrow_forward
- Imagine you observe a Cepheid variable star with an apparent V-band magnitude of 18.0 in the direction of the Andromeda galaxy which is at a distance of d = 850 kpc from us. The period of the star is 8 days and you know that the period-luminosity relation is My = −2.81 log P – 1.43. Verify if the star belongs to the Andromeda galaxy or not.arrow_forwardCalculate the total number density ( ntot ) and the density ( ρ ) at a depth in a star composed of pure hydrogen where T = 9500 K and 35 % of the atoms are ionized (assume UI = 2). What percentage of hydrogen atoms are in the energy level n = 2?arrow_forwardAn O8 V star has an apparent visual magnitude of +5. Use the method of spectroscopic parallax to estimate the distance to the star (in pc). (Hints: Refer to one of the H–R diagrams in the chapter, and use the magnitude–distance formula, d = 10(mV − MV + 5)/5 where d is the distance in parsecs, mV and MV are the apparent and absolute visual magnitude respectively.)arrow_forward
- You can estimate a star’s radius R(meters) by its luminosity L(Watts) and its surface temperature T(Kelvin) using L = 4πR2σT4, where σ = 5.670 × 10−8 (Wm−2K−4) is the Stephen-Boltzmann constant. Perform a first order error analysis (approximate the error in the function) of an estimate of a star’s radius when L = 9.273×1027W, ∆L = ±0.05L,T = 9400K, ∆T = ±0.02T. Calculate both the error and relative percent error.arrow_forward6arrow_forwardvelocity curve for a double line spectroscopic binary is shown in the sketch. The system is viewed edge-on, i.e., with an inclination angle of i 90°, so that the maximum possible Doppler shifts for this system are observed. 400 SPo = , Ain i 300 200 l0o = v Ain i 100 -100 -200 -300 400 0 1 2 3 4 10 Time (days) Find the speed of star 2 in km/s. Doppler Velocity (2esu)arrow_forward
- You receive 8 × 10−9 W/m2 of energy from a star that is 2 parsecs away, it has a V -band apparentmagnitude mV = −1.5. How much more/less flux do you receive from a star with an apparent magnitudemV = 5.3? For the first star, what is its V -band absolute magnitude?arrow_forwardPlasketts binary system consists of two stars that revolve in a circular orbit about a center of mass midway between them. This statement implies that the masses of the two stars are equal (Fig. P11.19). Assume the orbital speed of each star is |v|=220km/s and the orbital period of each is 14.4 days. Find the mass M of each star. (For comparison, the mass of our Sun is 1.99 1030 kg.)arrow_forwardA G0 III star with a mass of about 1 M⊙ sits on the horizontal branch. Horizontal branch stars are in the helium-burning phase of stellar evolution. For this process, 3He→C +energy If the star has a luminosity of 100 L⊙, estimate the size of this star assuming it has a temperature of 6000 K. What is the thermal time scale (time for the star to radiate away all its potential energy) if only 10% of the star’s mass is in the form of helium?arrow_forward
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