Foundations of Astronomy (MindTap Course List)
14th Edition
ISBN: 9781337399920
Author: Michael A. Seeds, Dana Backman
Publisher: Cengage Learning
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Chapter 11, Problem 11RQ
To determine
Explain the way in which geometry of bipolar flows and Herbig-Haro objects helps the hypothesis of existence of rotating disks around the protostar.
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Suppose two protostars form at the same time, one with a mass of 0.5MSunSun
[Select ALL answers that are true in alphabetical order]A) The 10MSun protostar will have a smaller change in surface temperature during this phase than the 0.5MSun protostar.B) The 10MSun protostar will reach the main sequence cooler and fainter than the 0.5MSun protostar.C) The 10MSun star will end its main-sequence life before the 0.5MSun star even completes its protostar stage.D) The 10MSun protostar will have a smaller change in luminosity during the sequence shown than the 0.5MSun protostar.E) The 10MSun protostar will be much more luminous than the 0.5MSun protostar.
Suppose a protostar has a luminosity of
157,341
Lo
and a surface temperature of 4,540 K
(Kelvins). What is the radius of this
protostar?
[Enter your answer as a multiple of the
Sun's radius. I.e., if you find R = 20
Ro
enter 20. This problem is easier if you
start with the relevant equation and
create a ratio using the Sun's values.
Recall that the Sun has a surface
temperature of 5778 K. ]
When a region of a molecular cloud collapses, a protostar is formed. How do the temperature and density change as a protostar gets smaller and smaller?
Group of answer choices
The temperature decreases and the density decreases.
The temperature decreases and the density increases.
The temperature increases and the density decreases.
The temperature increases and the density increases.
Chapter 11 Solutions
Foundations of Astronomy (MindTap Course List)
Ch. 11 - Prob. 1RQCh. 11 - Prob. 2RQCh. 11 - Prob. 3RQCh. 11 - Prob. 4RQCh. 11 - During free-fall collapse, what keeps the...Ch. 11 - Prob. 6RQCh. 11 - Prob. 7RQCh. 11 - Prob. 8RQCh. 11 - Prob. 9RQCh. 11 - Prob. 10RQ
Ch. 11 - Prob. 11RQCh. 11 - Prob. 12RQCh. 11 - Prob. 13RQCh. 11 - Describe the three ways thermal energy can be...Ch. 11 - Prob. 15RQCh. 11 - Prob. 16RQCh. 11 - How does the CNO cycle differ from the...Ch. 11 - Prob. 18RQCh. 11 - Prob. 19RQCh. 11 - Prob. 20RQCh. 11 - Prob. 21RQCh. 11 - Prob. 22RQCh. 11 - Prob. 23RQCh. 11 - Prob. 24RQCh. 11 - Prob. 1PCh. 11 - Prob. 2PCh. 11 - Prob. 3PCh. 11 - Prob. 4PCh. 11 - If a protostellar disk is 200 AU in radius and the...Ch. 11 - Prob. 6PCh. 11 - Prob. 7PCh. 11 - Prob. 8PCh. 11 - Prob. 9PCh. 11 - Prob. 10PCh. 11 - Prob. 11PCh. 11 - Prob. 12PCh. 11 - If the Orion Nebula is 8 pc in diameter and has a...Ch. 11 - Prob. 14PCh. 11 - Prob. 1SOPCh. 11 - Prob. 2SOPCh. 11 - Prob. 1LTLCh. 11 - Prob. 2LTLCh. 11 - Prob. 3LTLCh. 11 - Prob. 4LTLCh. 11 - Prob. 5LTLCh. 11 - Prob. 6LTL
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- Why is star formation more likely to occur in cold molecular clouds than in regions where the temperature of the interstellar medium is several hundred thousand degrees?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_forward12.1 In a certain part of the North American Nebula, the amount of interstellar extinction in the visual wavelength band is 1.1 magnitudes. The thickness of the nebula is estimated to be 20 pc, and it is located 700 pc from Earth. Suppose that a B spectral class main-sequence star is observed in the direction of the nebula and that the absolute visual magnitude of the star is known to be My = -1.1 from spectroscopic data. Neglect any other sources of extinction between the observer and the nebula. (a) Find the apparent visual magnitude of the star if it is lying just in front of the nebula. (b) Find the apparent visual magnitude of the star if it is lying just behind the nebula. Problems 443 (c) Without taking the existence of the nebula into consideration, based on its apparent mag- nitude, how far away does the star in part (b) appear to be? What would be the percentage error in determining the distance if interstellar extinction were neglected?arrow_forward
- Use the following formula (fitted to data) M = -4x10-13n gR Mo/year for the mass loss of asymptotic giant branch stars to: a) explain why L, g (gravity on surface), and R enter the equation the way they do (nominator or denominator). b) show that the expression for M is equivalent to LR M = -4x10-13n Mo/year M c) estimate the mass loss rate of a star with M = 1 Mo, L = 7000 Lo, T = 3000 K. Assume n = 1 and use the Stefan-Boltzmann equation to calculate R (in Ro).arrow_forwardwhy do dark streaks appear in visible light images of the Trifid nebula, but appear bright in an infared imagearrow_forwardConsider the image above of the Cassiopeia A (Cas A) supernova remnant. The supernova explosion that caused this remnant was observed on earth about 300 years ago. It is about 3000 pc away. Since that time, the shockwave from the supernova has expanded to form the roughly spherical cloud pictured above. From the center point to the edge of the cloud is about 3 pc. Compute the angular diameter of the Cas A supernova remnant as viewed from Earth. Express your answer in arcminutes.arrow_forward
- A planetary nebula expanded in radius 0.3 arc seconds in 30 years. Doppler measurements show the nebula is expanding at a rate of 35 km/s. How far away is the nebula in parsecs? First, determine what distance the nebular expanded in parsecs during the time mentioned. Δd = vpc/sTs So we first need to convert the rate into pc/s and the time into seconds: vpc/s = vkm/s (1 pc / 3.09 x 1013km) vpc/s = ? Ts = (Tyr)(365 days/yr)(24 hrs/day)(3600 s/hr) Ts = ? s Δd= vpc/sTs Therefore, Δd = ? pcarrow_forwardPlease give answer. Describe, with the aid of suitable diagrams, the basic structure and components of the ATLAS detector at the LHC.arrow_forwardresult, the -1 from a T Tauri star, estimate the mass density of the wind at a distance of 100 AU from the star. (Hint: Refer to Example 11.2.1.) Compare your answer with the density of the giant molecular cloud agpalain Example 12.2.1. 12.19 Assuming a mass loss rate of 10-7 Mo yr¹ and a stellar wind velocity of 80 km s -niem-1299 eararrow_forward
- How many years? Thank you!arrow_forwardc) The star may be assumed to evolve with effective temperature, Teff, remaining constant. Show that the time, t₁, taken by such a star to evolve from a large radius to some smaller radius, R₁, is given by where L₁ is the luminosity when the star has radius R₁. t₁ = GM² 7L₁R₁'arrow_forwardExplain what makes the planetary nebula glow and what makes the supernova remnant glow. Which of these two kinds of gas clouds continues to glow for a longer time and why?arrow_forward
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