2018 astronomy science Olympiad – Flashcards

(Slide 9) A region where radiation from hot, young stars is energizing the surrounding gas and dust, about 6,500 light years away an HII area, radiation from hot, young stars strip away the electrons from neutral hydrogen atoms to form clouds of ionized hydrogen

(Slide 11) 3000 light years away in the constellation of Cepheus, star formation that has hot new stars producing powerful winds that form the columns and pillars

A luminous blue variable star which is losing mass 7 x 10^ km/hr winds caused it, bright glare in center is not the star white cross is glitch from Hubble's wide field and planetary camera 2

(Slide 12) largest yellow hyper giant detected, hyper giants are among the largest stars in the universe with enormous mass and luminosity and unstable with an extremely high rate of mass loss, this star has a companion star that is 2.8 AU away from it, eclipses main star every 1300 days the distance of the center of the first star to the center of the second star is 10 AU

(Slide 14) prototype for the S Doradus class of variable stars, also known as luminous blue variable one of the brightest stars brightest in the Large Magellanic Cloud. Extremely massive and luminous and has a stellar wind blowing sway significant portions of its mass resembles an F-type supergiant

(Slide 16) red supergiant 4.5 AU in diameter, a semi regular pulsating variable, it has been shedding gas and dust that forms a nebula 400 AU in diameter

(Slide 17) a Type II supernova remnant, x-ray, optical composite stellar core is slowest spinning neutron star ever detected, rotating once every 6.5 hours compared to several times a minute for other neutron stars, it is a magnetar

(Slide 18) May have the Milky Way Galaxy's youngest black hole in the center, images are x-ray, radio, Infrared, and a composite of the three images, the flattened ends of the x-ray jets rich in iron and nickel produced during the collapse are produced by the jets running into a dense cloud of Gas and dust, an ejects dominated remnant with evidence of a stratified distribution of elements (iron in center, and silicon and sulfur in outer regions) detection of a jet and the non-detection of a neutron star make it a candidate for a gamma-ray burst remnant with a black hole

(Slide 19) A supernova remnant in the direction of the constellation Gemini, it has a neutron star stellar core, but it is not in the center of the remnant, the pulsar JO617 (which is in The Nebula) is misaligned from the remnant so maybe it is not associated with the Nebula or maybe there is movement towards the left of the materials in the remnant pushing JO617's cometary tail to one side

(Slide 20) Discovered on February 23, 1987 in the Large Magellanic Cloud, it showed the phases, before, during, and after the collapse of a massive star, a ring of gas surrounding the supernova around 20,000 years before the collapse is the diameter of one Light year and glows in optical light central structure is half a light year the clumps of debris are moving at 20 x 10^6 miles per hour, the shock wave has moved through and beyond the ring of gas into a less dense gas region, the collapse of the progenitor star has created vast amounts of dust , a flash of neutrinos was detected so there could be a neutron star or black hole in the center of the area

(Slide 2q) A supernova event that is 3 x 10^9 light years away and produced twice the power of any previous supernova, but the light from it started dimming only three months after it occurred, even though optical radiation continued to fade, the UV radiation increase fivefold where it reigned for two months before starting to fade, strong emission lines would be present if shock wave was interacting with its own ejects but that is not occurring, so there might be a magnet at in the center, but it does not explain the resurgence of UV radiation

(Slide 22) The first unidentified gamma-ray source PSR BO355+54 and this are pulsars with very different shapes and structures. Some pulsars generate pulsar wind nebulas of high energy particles. The shapes of these pulsar wind nebulas (PWNs) may explain the presence or absence of radio and gamma-ray pulses. Both pulsars rotate 5 times/second and are 500,000 years old. Geminga has gamma-ray pulses with no bright radio emissions and BO355+54 is one of the brightest radio pulsar known but is not observable in gamma rays. study of the orientation of the donut-shaped disk jetsdemonstrates why the radio emissions from Geminga and the gamma-ray emissions from B0355+54 are orientated away from our line of sight and therefore not visible.

(Slide 23) an ultra luminous X-ray source (ULX) located in the galaxy M82 12 x 10^6 light years away, a pulsar that rotates every 1.37 seconds and revolves around about a 5.2 solar mass companion in a binary star system, the brightest pulsar ever recorded NuSTAR detected pulsations which are associated with pulsar and the Chandra data helped determine the exact source of the pulsations and therefore the location of the pulsar.

(Slide 24) an X-ray binary system consisting of a neutron star and massive companion it is 30,700 light years away , arises that if it is twice as far away its energy output is twice as much as thought which leads to the implication that the system has exceeded the Eddington Limit - the balance between gravity in and radiation pressure out. It is thought that this limit can only be exceeded by black holes - not neutron stars. The extreme velocity of the high-energy particles produced by the system are at least 99.9% the speed of light

(Slide 25) An HII region located in the Large Magellanic Cloud, yellow and Cyan from the MCLS telescope in Chili traces the HII emission from DEM L241, the observational data shows an X-ray point likely to be a neutron star or black hole and a massive star which survived the catastrophic collapse of the companion, the progenitor Star was between 25 and 40 solar masses, this might be the third system containing both a massive star and a neutron star or black hole found in the aftermath of a supernova

V = H0 D where V= observed velocity of the galaxy away from us in km/sec, H is Hubble's constant which is 70 km/sec/Mpc and D= distance

T = (2.898 x 10^6)/(lamda max) T = temperature in Kelvin, lamda = Max wavelength remission in nanometers

P = eoA(T)^4 P = power radiated (watts) e = emissary ( no units) A = surface area (m^2) T = temperature (in Kelvin)

When T = 12000 K, lamda Max = 250 nm (blue) when T = 6000 K, lamda Max = 500 nm (yellow) , when T = 3000 K, lamda Max equals 1000 m (red) as the wavelength (lamda) increases, the brightness decreases

M = m - 5 log ((r)/(10))

(MA + MB) = (a)^3/(p)^2

vP

m (a of c)

V^2 / r

D = (ad)/(206,265)

206,265 au or 3.26 light years or 3.08 x 10^16 meters

60 arcmin = 60'; 1' = 60 arcsec = 60"

L =1/h(r)^2