They both have huge growth of vegetation and are both extremely humid with good amounts of rain
Answer:
sympatric speciation
Explanation:
Species of fruit fly larvae in the genus Rhagoletis each feed on a particular kind of fruit. Rhagoletis pomonella feeds on the small red fruit of the hawthorn tree. In 1865, farmers in the Hudson River valley found that R. pomonella flies had begun attacking their apples and then spread to apple orchards in adjacent areas of Massachusetts and Connecticut. These now separate varieties of flies, the apple and haw flies, usually don't interbreed with each other because their periods of mating coincide with the different ripening times of apples and hawthorn fruit. Each variety is becoming specialized to feed and reproduce in its own particular microhabitat and may be transitioning to separate species.If the apple and haw flies become distinct enough to be separate species, their evolution is an example of sympatric speciation
Answer:
Explanation:
Using the Mendelian approach to solve this question, we will understand that the mendelian approach has a pattern for inherited traits.
From the data set given, the total number of the population is:
43+9+32+110 = 194
However, their ratio are being calculated as follows:
43/194 = 0.22
9/194 = 0.05
32/194 = 0.16
110/194 = 0.57
After comparison with the Mendelian's approach, we realize that these results seem to be similar to the 9:3:3:1 ratio.
i.e.
3/16 = 0.18
1/16 = 0.06
3/16 = 0.18
9/16 = 0.56
The inheritance pattern obviously dictates that the flax experiment proceeds in the pattern found in the Mendelian's Approach and the resistance of the two different strains were arbitrated by two traits.
A. umbilical cord is the answer
Gravity
Neutron stars are the most extreme and fascinating objects known to exist in our universe: Such a star has a mass that is up to twice that of the sun but a radius of only a dozen kilometers: hence it has an enormous density, thousands of billions of times that of the densest element on Earth. An important property of neutron stars, distinguishing them from normal stars, is that their mass cannot grow without bound. Indeed, if a nonrotating star increases its mass, also its density will increase. Normally this will lead to a new equilibrium and the star can live stably in this state for thousands of years. This process, however, cannot repeat indefinitely and the accreting star will reach a mass above which no physical pressure will prevent it from collapsing to a black hole. The critical mass when this happens is called the "maximum mass" and represents an upper limit to the mass that a nonrotating neutron star can be.
However, once the maximum mass is reached, the star also has an alternative to the collapse: it can rotate. A rotating star, in fact, can support a mass larger than if it was nonrotating, simply because the additional centrifugal force can help balance the gravitational force. Also in this case, however, the star cannot be arbitrarily massive because an increase in mass must be accompanied by an increase in the rotation and there is a limit to how fast a star can rotate before breaking apart. Hence, for any neutron star, there is an absolute maximum mass and is given by the largest mass of the fastest-spinning model.
