Answer to Question 1
True
Answer to Question 2
The upper end in the main sequence of the H-R diagram shows that even if an extremely massive star does begin to form, stellar models reveal that such massive stars are unstable. To support the tremendous weight in such stars, the internal gas must be very hot, and that means it must emit floods of radiation that flow outward through the star. The resulting pressure of the radiation blows gas away from the star's surface in powerful stellar winds. The models indicate, for example, that a 60-solar- mass star sheds mass so rapidly that it can be reduced to less than 30 solar masses in only a million years.
Pili extending from the surface of Proteus mirabilis.
Surface of the heart.
Development encompasses both gains and losses. Sometimes a health crisis (loss) can result in a heal
How to find the volume and surface area a rectangular prism
The striking structural similarity between the translocation factor EF-G (right) and the ternary
Observed global land and ocean surface temperature anomalies since 1850