arXiv:1404.0641v2 [astro
... of hosts younger than 3 Gyr represents that very fraction of Pop I stars that would be born provided the star formation rate is nearly constant during the whole period of the thin disk formation. One of the biggest sources of the latest generation of stars in the Milky Way is the Orion nebula, where ...
... of hosts younger than 3 Gyr represents that very fraction of Pop I stars that would be born provided the star formation rate is nearly constant during the whole period of the thin disk formation. One of the biggest sources of the latest generation of stars in the Milky Way is the Orion nebula, where ...
Thermally induced structural rearrangement of the Fe(ii)
... The thermal stability, one of the key properties for a commercially successful electrochromic material, is in the scope of the present study. Studies on thin films of neat Fe-MEPEs showed that annealing above 100 1C leads to an irreversible colour change from blue to green and a loss of the electroc ...
... The thermal stability, one of the key properties for a commercially successful electrochromic material, is in the scope of the present study. Studies on thin films of neat Fe-MEPEs showed that annealing above 100 1C leads to an irreversible colour change from blue to green and a loss of the electroc ...
Large scale kinematics and dynamical modelling of the Milky Way
... McGinn et al. (1989) had large scattering in their data. Hence the Milky Way nuclear star cluster kinematics are known in detail at small scales, but the large scale kinematics beyond 1 pc remain uncertain. For example, the rotation is not yet well determined, although a rotation law can provide ins ...
... McGinn et al. (1989) had large scattering in their data. Hence the Milky Way nuclear star cluster kinematics are known in detail at small scales, but the large scale kinematics beyond 1 pc remain uncertain. For example, the rotation is not yet well determined, although a rotation law can provide ins ...
No. 2 - Society for Astronomical Sciences
... are likely to appear in upcoming publications about the eruption. Olivier Thizy presented a practical – and ongoing – example of pro-am collaboration in spectroscopy focused on the Be stars. These are hot “B” stars whose spectral lines change from emission to absorption as the star cycles. Amateur r ...
... are likely to appear in upcoming publications about the eruption. Olivier Thizy presented a practical – and ongoing – example of pro-am collaboration in spectroscopy focused on the Be stars. These are hot “B” stars whose spectral lines change from emission to absorption as the star cycles. Amateur r ...
Astronomy 3130 Spring 2014 Observation Lab 2 vs.
... b) Observe and quantify the Airy pattern for different telescope apertures: Find a bright star within 30-40 degrees of the zenith (to minimize the blur due to seeing). Pollux should work well this time of year. For the 6”, 4”, 2”, 1” and 0.5” apertures make observations of the “size” of the star im ...
... b) Observe and quantify the Airy pattern for different telescope apertures: Find a bright star within 30-40 degrees of the zenith (to minimize the blur due to seeing). Pollux should work well this time of year. For the 6”, 4”, 2”, 1” and 0.5” apertures make observations of the “size” of the star im ...
Stellar Evolution and the fate of the Solar System
... YUV420 codec decompressor are needed to see this picture. ...
... YUV420 codec decompressor are needed to see this picture. ...
Another cluster of red supergiants close to RSGC1
... Aims. We analyse a previously unreported concentration of bright red stars ∼16 away from the cluster RSGC1 Methods. We utilised near IR photometry to identify candidate red supergiants and then K-band spectroscopy of a sample to characterise their properties. Results. We find a compact clump of eig ...
... Aims. We analyse a previously unreported concentration of bright red stars ∼16 away from the cluster RSGC1 Methods. We utilised near IR photometry to identify candidate red supergiants and then K-band spectroscopy of a sample to characterise their properties. Results. We find a compact clump of eig ...
A) Polaris B) Betelgeuse C) Procyon B D) Sirius 1. Which star has a
... A) in the Sun by fusion B) when water condenses in Earth's atmosphere C) from the movement of crustal plates D) during nuclear decay 23. Base your answer to the following question on the diagram below, which shows an inferred sequence in which our solar system formed from a giant interstellar cloud ...
... A) in the Sun by fusion B) when water condenses in Earth's atmosphere C) from the movement of crustal plates D) during nuclear decay 23. Base your answer to the following question on the diagram below, which shows an inferred sequence in which our solar system formed from a giant interstellar cloud ...
L17 SHELL-SHOCKED DIFFUSION MODEL FOR THE LIGHT
... expansion timescale is just texp ⯝ (DR/vexp ) for constant expansion speed. In a thermal diffusion model for SN 2006gy, we take the light-curve peak at 70 days (Smith et al. 2007) as representative of both tdiff and texp. From the observed constant expansion speed of vexp ⯝ 4000 km s⫺1 (Smith et al. ...
... expansion timescale is just texp ⯝ (DR/vexp ) for constant expansion speed. In a thermal diffusion model for SN 2006gy, we take the light-curve peak at 70 days (Smith et al. 2007) as representative of both tdiff and texp. From the observed constant expansion speed of vexp ⯝ 4000 km s⫺1 (Smith et al. ...
(FT-IR) Microspectroscopic Measurements of Intact Spheres
... the material as an idealized object, such as a sphere, and largely neglects the optical configuration of the microscope and spectrometer. Success has been reported in using this approach to understand the spectra of complex tissues as well as that of spheres themselves.9,10 In another line of inquir ...
... the material as an idealized object, such as a sphere, and largely neglects the optical configuration of the microscope and spectrometer. Success has been reported in using this approach to understand the spectra of complex tissues as well as that of spheres themselves.9,10 In another line of inquir ...
Radio Astronomy in the Early Twenty
... centimeter wavelengths have received increasingly prominent consideration. This activity results from the need for greater sensitivity and higher survey speed, required to pursue a range of astronomical and cosmological questions. The high angular resolution provided by very long baseline interferom ...
... centimeter wavelengths have received increasingly prominent consideration. This activity results from the need for greater sensitivity and higher survey speed, required to pursue a range of astronomical and cosmological questions. The high angular resolution provided by very long baseline interferom ...
Overview Evolution of massive stars Evolution of massive stars
... The shock from the supernova is traveling outward at about 10% the speed of light. The ejecta carrys the newly synthesized elements with it into the interstellar medium, ready to become the next generation of stars. When the shock encounters a stable gas cloud it mixes metals into the gas cloud, and ...
... The shock from the supernova is traveling outward at about 10% the speed of light. The ejecta carrys the newly synthesized elements with it into the interstellar medium, ready to become the next generation of stars. When the shock encounters a stable gas cloud it mixes metals into the gas cloud, and ...
Title Goes Here
... In order to clarify such fundamental properties by optical spectroscopy, we need to measure both emission and absorption spectra at various temperatures and electron densities. This is because emission and absorption in doped systems selectively occur for occupied and unoccupied conduction-band stat ...
... In order to clarify such fundamental properties by optical spectroscopy, we need to measure both emission and absorption spectra at various temperatures and electron densities. This is because emission and absorption in doped systems selectively occur for occupied and unoccupied conduction-band stat ...
Summary of Astronomy
... at the University of Alaska Fairbanks. Akasofu has studied the aurora since 1957, and he thinks other planets' auroras could be used to detect life elsewhere in the universe. The idea was inspired by the discovery of three planets circling a sun that's much like ours, though a bit bigger. The star, ...
... at the University of Alaska Fairbanks. Akasofu has studied the aurora since 1957, and he thinks other planets' auroras could be used to detect life elsewhere in the universe. The idea was inspired by the discovery of three planets circling a sun that's much like ours, though a bit bigger. The star, ...
Reid_may
... Over 150 extrasolar planets have been discovered since 1995 -this includes several multiplanet systems 1. Are there any properties (besides [m/H]) that set the parent stars apart from the average disk star? 2. Given the statistical properties of the parent stars, coupled with our current knowledge o ...
... Over 150 extrasolar planets have been discovered since 1995 -this includes several multiplanet systems 1. Are there any properties (besides [m/H]) that set the parent stars apart from the average disk star? 2. Given the statistical properties of the parent stars, coupled with our current knowledge o ...
The Resolving Power Of a Microscope and Telescope
... match the refractive index of glass slides used. (This limits reflection from slides). Thus the numerical aperture is limited to just 1.4-1.6. Thus, optical microscopes (if you do the math) can only image to about 0.1 micron. This means that usually organelles, viruses and proteins cannot be imaged. ...
... match the refractive index of glass slides used. (This limits reflection from slides). Thus the numerical aperture is limited to just 1.4-1.6. Thus, optical microscopes (if you do the math) can only image to about 0.1 micron. This means that usually organelles, viruses and proteins cannot be imaged. ...
Kinematics of Arp 270: gas flows, nuclear activity
... might well expect distinct star formation regimes within them. We have initiated a programme of kinematic observations of interacting galaxy pairs analysing the Hα emission line, using an instrument which gives unequalled angular and velocity resolution per unit observation time. These observations, ...
... might well expect distinct star formation regimes within them. We have initiated a programme of kinematic observations of interacting galaxy pairs analysing the Hα emission line, using an instrument which gives unequalled angular and velocity resolution per unit observation time. These observations, ...
THE GREAT AGN DEBATE `AGN VS STARBURST
... Generally galaxies undergo a period of star formation after a collision or close encounter between two galaxies. ‘The tidal forces between the two galaxies disrupt gas and cause it to fall inward, greatly accelerating the normal process by which interstellar clouds collapse and form stars’ (Weaver, ...
... Generally galaxies undergo a period of star formation after a collision or close encounter between two galaxies. ‘The tidal forces between the two galaxies disrupt gas and cause it to fall inward, greatly accelerating the normal process by which interstellar clouds collapse and form stars’ (Weaver, ...
Magnetic fields in O-, B-and A-type stars on the main sequence
... An explanation of the observed fields of Ap stars already proposed a long time ago is the fossil origin. The fossil origin suggests that magnetic fields reside inside the star without being continuously renewed. Therefore, these fields have been formed during an early phase of the life of the star. ...
... An explanation of the observed fields of Ap stars already proposed a long time ago is the fossil origin. The fossil origin suggests that magnetic fields reside inside the star without being continuously renewed. Therefore, these fields have been formed during an early phase of the life of the star. ...
Astronomical spectroscopy
Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects. Spectroscopy can be used to derive many properties of distant stars and galaxies, such as their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using Doppler shift measurements.