Rr Lyrae Research Paper

I pick the star Antares, from the H-R diagram I can tell that it it is a Red Supergiant, and it has a surface temperature that is around 3,000 degrees kelvin, which is cooler than the Sun by at least 2,000 degrees kelvin, but its luminosity is around 10,000 solar units, which means it produces much more energy than our Sun does, so it is a lot brighter. The spectral type of Antares is a M, I could tell that its spectral type was M because I read the H-R Diagram, the VLab told me that the star ‘Betelgeuse’ has a spectral type of M, and Antares is right below, and basically inside Betelgeuse. Stars with the same spectral type have the same chemical composition, so Antares has the chemical composition Ca (calcium), TiO (titanium oxide), CH (methylidene).

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

In this paper I will explain how astronomers determine the composition, temperature, speed, and rotation rate of distant objects using various methods. I will explain the properties of stars. I will also summarize the complete lifecycle of the Sun and determine where the Sun is currently in its lifecycle.

They are very luminous stars that have a relatively cool surface temperature compared to the stars in the main sequence that have about the same luminosity. Red giants typically have low to intermediate mass than a regular star, even though they are about 1000 times larger in the red giant phase of stellar evolution. Red supergiants are known as the biggest stars by radius. The biggest red supergiant is mentioned as VY Canis Majoris. This star is about 1800 times bigger than our sun. Although there are plenty of red giants in space, none of them are that close to us. The closest red giant is Gamma Crucis (88 light years away).3

Parenago 1802, a member of the ∼1 Myr Orion Nebula Cluster, is a double-lined, detached eclipsing binary in a 4.674 d orbit, with equal-mass components (M2/M1=0.985±0.029). Here we present extensive V IC JHKS light curves spanning ∼15 yr, as well as a Keck/HIRES optical spectrum. The light curves evince a third light source that is variable with a period of 0.73 d, and is also manifested in the high-resolution spectrum, strongly indicating the presence of a third star in the system, probably a rapidly rotating classical T Tauri star. We incorporate this third light into our radial velocity and light curve modeling of the eclipsing pair, measuring accurate masses (M1=0.391±0.032, M2=0.385±0.032 M⊙), radii (R1=1.73±0.02, R2=1.62±0.02 R⊙), and temperature ratio (Teff,1/Teff,2=1.0924±0.0017). Thus the radii of the eclipsing stars differ by 6.9±0.8%, the temperatures differ by 9.2±0.2%, and consequently the luminosities differ by 62±3%, despite having masses equal to within 3%. This could be indicative of an age difference of ∼ 3 × 105 yr between the two eclipsing stars, perhaps a vestige of the binary formation history. We find that the eclipsing pair is in an orbit that has not yet fully circularized,

The life cycle of the star is a long process that has taken place for billions of years and will continue to take place long after our star is no longer in existence. In this essay I will be explaining the magnificent process of how a star is first born till the end of its life cycle. First, I will be explaining how the star is first formed in all its beauty big or small. Then, I will be explaining the path of an average star like our own sun will take. After, I will be explaining the journey of a massive star in all its glory till its destructive end. All stars are first formed in clouds of gas called nebulae, turbulence deep within the nebulae causes cores to form as the mass begins to grow the nebulae begins to collapse upon itself due to

Guillem Anglada-Escud´e, Pamela Arriagada, Steven S. Vogt, Eugenio J. Rivera, R. Paul Butler, Jeffrey D. Crane, Stephen A. Shectman, Ian B. Thompson, Dante Minniti, Nader Haghighipour, Brad D. Carter, C. G. Tinney, Robert A. Wittenmyer, Jeremy A. Bailey, Simon J. O’Toole, Hugh R.A. Jones, James S. Jenkins

Next, there are the observations of novae. Novae are stars that show a sudden increase in brightness before returning back to their original

It is the brightest astronomical radio source in the sky. It was discovered in 1947 and is the strongest radio source outside the solar system. Its explosion ejected cloud material that is 10 light years across and is expanding at a rate of 4,000-6,000 km/s. Its temperature s about 50 million degrees F. The first light of this supernova reached us about 300 years ago! Coordinates: RA 23h 23m 26.7s | Dec +58° 49' 03.00"

A nebulae as described in Fraknoi’s Voyages to the Stars and Galaxies is “all objects that were not sharp points of light” (Fraknoi, page 384). The Sagittarius Triplet is a group of three nebulae’s famous for their bright red and blue hues, which is a main reason I choose this picture. There are three nebulae in this picture and each is spectacular on its own but together the Sagittarius Triplet creates a visual buffet for the eyes. The dark reds in particular are beautiful to behold and take up the majority of the visual landscape. These red colors are created by the emission nebulae by hydrogen gas that is heated by the intense temperatures of present stars. The image made me feel the vastness of space and the endlessness of time. The interesting layout of the nebulae creates a long stardust highway across the image, connecting the NGC 6559 and M8 nebulae. These three nebulae are so bright they are routinely featured in telescopic tours of the Sagittarius constellation and the central Milky Way galaxy. M8 or the Lagoon Nebula and M20 or Trifid were first cataloged in 1764 by Charles Messier (Kronberg).

Stars go through phases with each one altering the star. They start as a protostar then ignite to

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.

may occur in groups of up to 10 or less (see figure 2) and occur in pairs parallel to the equator with the magnetic field of one directed into the sun, and the other pointing out

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.

variant from light blue to shades of grey and pulsates between 15 and 20 cycles per minute. The