Key Properties Of Galaxy Clusters

After a time, the hydrogen runs out almost completely, and it collapses. New reactions begin to take place in the core and these reactions cause the star to expand rapidly. As the stars begin to deplete their new fuel, they switch to others. New elements are formed in the cores of stars but they become too heavy. The star has reached its end growth. When it reaches the end, a tremendous amount of energy is released and it begins to shed its outer layers, the gravity is too weak hold onto them anymore. Once the layers are removed, in the stars place is a fiery core called a planetary nebula. Eventually, the core runs out of fuel and it collapses. This star is now in a very dense state, and is called a white dwarf. Eventually, the white dwarf cools until it no longer shines. This dead star is called a brown dwarf.More massive stars, however, have more violent ways of dying. Some stars turn it into a supergiant. Supergiant stars are extremely bright, and are extremely large. Supergiant stars cores, can collapse violently and suddenly. This collapse causes a tremendous explosion, called a

Procedure: Have you made any changes to the procedure? Please explain. If you made no changes, state so. (1 point)

The Nebular hypothesis began as a cloud. The cloud starts to compact as it cools. The Law

The area on the H-R diagram where “normal” stars can be found is known as the _________.

Curtis correctly noted that spectral lines could be seen within the spiral nebulae, and that they were generally consistent with the nebulae in the form of large assembled star clusters. These clusters supported Curtis's argument that these were in fact stellar systems, which are comparable to our Milky Way

What probably has been the core of the “target” galaxy can be seen as a small yellow area at 5 o’clock inside the newly formed ring. Massive star formation dominates the ring. Infrared observations also reveal a strong

Simulations of galaxy formation based on the Lambda Cold Dark matter (ΛCDM) cosmological model predict that a large galaxy such as the Milky Way should have many (~ 200) dwarf satellite galaxies. However, only about 20 or 30 have been identified. Where are the rest? Warm dark matter, constituting of sterile neutrinos, is lighter and since dwarf galaxies consisting mainly of dark matter are so difficult to find by visible light, there could be enough of them to reconcile the large number of dwarf galaxies that simulations predict to exist with the small number actually observed. We are looking for a weak unidentified emission line at E = (3.55−3.57) ±0.03 keV in a stacked XMM-Newton spectrum of Dwarf galaxies, which are the satellite galaxies of our Milky Way.

The cloud contracted under its own gravity and our proto-Sun formed in the hot dense center. The remainder of the cloud formed a swirling disk call the solar nebula. A solar nebula is a gaseous cloud. The nebular hypothesis has become the theory of the origin of our solar system. We can relate this to the vermiculite solar nebula lab. These are related because in the lab it showed us how gravity pulled most of the materials toward the center of the water which the water was representing gravity and the vermiculite that got pulled to the center was modeling the heavier more dense planets. The vermiculite that was pushed away from the center represented lighter less dense

ligible proper motion of the G.S. is a good indication that the HST field stars47 are expected

“Active galactic nuclei” are objects occupying the center of many galaxies that consist of an accreting supermassive black hole and are some of the most luminous and powerful bodies in our known Universe. In the galactic-BH accretion process, gaseous matter from the galaxy is pulled into the black hole and is converted to into radiation that is then released radially outward into the host galaxy. Due to the rapid-fire accretion onto the Supermassive Black Hole, Active Galactic Nuclei (AGN) can emit radiation into their host galaxies that span much of the electromagnetic spectrum from X-rays, IR, UV, and radio waves. Researchers have organized AGN into groups based on their

M98 is an intermediate spiral galaxy, it is located approximately 44.4 million light years away in the Coma Berenices constellation. The M98 was found by the French astronomer Pierre Méchain in 1781. Messier 98 has a blue shift, a right ascension of 12:13.8 (h:m), a declination of +14:54 (deg:m), a distance of 60000 (kly), a visual brightness of 10.1 (mag) and an apparent dimension of 9.5x3.2 (arc min). The morphological classification of this galaxy is SAB(s)ab.

It is the first time scientists have measured the effect that pulsating, older red stars have on the light of their surrounding galaxy. The findings are published in the November 16 online edition of the journal Nature.

In lab six our topic was a continued learning about the Herstsprung-Russell diagram. We will discuss the properties needed to plot an open cluster of stars called the Pleiades cluster. Using the HR diagram we identified the temperature, age and characteristics of these main sequence stars. We applied all of this data and plotted it on our own diagram. From there we answered questions about different results that were found.

First observed in the early 70's \citep{Giacconi71, Tananbaum72}, the APPs are the brightest objects in the X-ray sky. Their powerful electromagnetic radiation is powered by the gravitational potential energy of the accreted matter. The accreting matter is directed by the magnetosphere onto the the magnetic poles of the star, thereby increasing its energy and angular momentum in the process. The rapid slowdown of the accreting matter at the polar surface of the star releases gravitational potential energy as X-rays, and the rotation of these X-ray hot spots across our line of sight gives rise to the observed periodic

Finally, Figure 3 shows Messier 46. This is an open cluster in the constellation of Puppis, which is roughly 5400 light years away. This makes it the closest of the objects by far. As it is an open cluster, there is no clear center of the object. This makes it slightly easier to analyze, as there is no center of light obscuring the individual stars. If we compare it to an image from Jose Luis Martinez, shown below, we can see that there are not too many differences. It is clear that the star structure is very similar, and while Jose’s image is more zoomed and enhanced, there are only a few more stars visible in his. We can see in both images that the stars towards the center of the cluster are slightly larger and more luminous, and it would