A) They are two names for the same entity.
B) In giant molecular clouds, H II regions surround ultraviolet-emitting stars (types O andB) , which have ionized the hydrogen around them.
C) In H II regions, giant molecular clouds are concentrations of other molecules like CO and H2O.
D) Giant molecular clouds evolve into H II regions as the molecules other than hydrogen are used up in star formation.
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A) lower right.
B) upper left.
C) lower left.
D) upper right.
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A) the light isotope of helium, 3He.
B) heavy hydrogen, 2H.
C) beryllium, 8Be.
D) carbon, 12C.
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A) The core cools down and contracts.
B) The core expands and cools down.
C) The core heats up and expands.
D) The core contracts and heats up.
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A) toward the upper right
B) toward the lower left
C) toward the lower right
D) toward the upper left
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A) emission nebulae
B) reflection nebulae
C) dark nebulae
D) planetary nebulae
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A) explosion of a star at the end of its life, the supernova phenomenon.
B) overcoming of gas pressure by self-gravity in a cold and dense interstellar cloud, to form a star.
C) conditions under which sufficient numbers of neutrinos can trigger the collapse of an interstellar cloud.
D) expansion of a gas cloud after gravitational contraction because of buildup of great heat within the cloud from gravitational potential energy.
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A) about 5 times its present diameter
B) about 15 times its present diameter
C) about 50 times its present diameter
D) same diameter it has now
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A) One star can be enshrouded in an accretion disk.
B) The gravitational force of one star will make its companion move in an orbit rather than remaining stationary.
C) Intense radiation from a hot star can produce nuclear reactions on the surface of a cooler companion and initiate a nova explosion.
D) Mass can be transferred from one star to its companion.
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A) 1 billion years
B) 1 million years
C) 1011 years
D) 1010 years
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A) about 1/4
B) less than 10 percent
C) about 1/2
D) about 3/4
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A) upward and toward the right.
B) downward and toward the left.
C) upward and toward the left.
D) downward and toward the right.
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A) in the red giant stage, before the helium flash
B) during and immediately after the (first) red giant or supergiant stage
C) during the protostar stage
D) after the main-sequence phase, before the star becomes a red giant
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A) gamma ray
B) ultraviolet
C) infrared
D) X-ray
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A) gravitational energy released as the protostar expands.
B) nuclear reactions in its core converting helium to carbon and oxygen.
C) gravitational energy released as the star contracts.
D) nuclear reactions in its core converting hydrogen into helium.
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Multiple Choice
A) 10 times the size of the solar system and contain 2 to 3 solar masses of material.
B) 10 pc across and contain a few thousand solar masses of material.
C) 100 pc across and contain 2 million solar masses of material.
D) 1000 pc across and contain 100 million solar masses of material.
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A) when it becomes a main-sequence star
B) when it leaves the main sequence
C) when it becomes a protostar
D) This question has different answers for stars of different masses. Massive stars never achieve equilibrium; small stars achieve hydrostatic equilibrium as soon as they reach the main sequence.
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A) hydrogen fusion
B) helium fusion
C) carbon fusion
D) silicon fusion
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A) about 450
B) at least a million, but less than 100 million
C) at least 100 billion
D) at least 100 million, but less than 100 billion
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A) larger and hotter.
B) hotter but not necessarily larger.
C) cooler but not necessarily larger.
D) larger and cooler.
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