The Official Magazine of the University Of St Andrews Astronomical Society 1
... At this stage in the stars’ lives the stars are surrounded by a disk of material within which the cores of gas giants are forming. At this point, rocky planets have not begun to form yet. The giant flares are long enough to reach the inner edge of the disks, and hence interact with the disks. Right ...
... At this stage in the stars’ lives the stars are surrounded by a disk of material within which the cores of gas giants are forming. At this point, rocky planets have not begun to form yet. The giant flares are long enough to reach the inner edge of the disks, and hence interact with the disks. Right ...
July2006_NL
... planets orbiting about the Sun. Surprisingly, the velocity tends to flatten out to a nearly constant value at large distances from the center. Thus a star in the middle part of the galaxy would have nearly the same speed as a star on the outer edge, as shown in Figure 1-2. Astronomers have tried to ...
... planets orbiting about the Sun. Surprisingly, the velocity tends to flatten out to a nearly constant value at large distances from the center. Thus a star in the middle part of the galaxy would have nearly the same speed as a star on the outer edge, as shown in Figure 1-2. Astronomers have tried to ...
The K2-ESPRINT Project III: A Close-in Super
... high galactic latitude (+60◦ ) and samples a distinct stellar population from the prime Kepler mission. Our target is labeled as EPIC 206318379 (which we call K2-28 hereafter) with the Kepler magnitude of mKep = 14.854. The relative brightness of the star in the near infrared (e.g., mH = 11.03) summ ...
... high galactic latitude (+60◦ ) and samples a distinct stellar population from the prime Kepler mission. Our target is labeled as EPIC 206318379 (which we call K2-28 hereafter) with the Kepler magnitude of mKep = 14.854. The relative brightness of the star in the near infrared (e.g., mH = 11.03) summ ...
Annual Report 2014 - Max Planck Institute for Astrophysics
... the directorship of Ludwig Biermann. It was estab- MPA has had an internationally-recognized numerlished as an offshoot of the Max-Planck-Institut für ical astrophysics program that was long unparalPhysik, which at that time had just moved from leled by any other institution of similar size. Göttinge ...
... the directorship of Ludwig Biermann. It was estab- MPA has had an internationally-recognized numerlished as an offshoot of the Max-Planck-Institut für ical astrophysics program that was long unparalPhysik, which at that time had just moved from leled by any other institution of similar size. Göttinge ...
Ray Optics at a Deep-Subwavelength Scale: A Transformation Optics Approach Seunghoon Han,
... by finding low-loss negative index materials25,26 or introducing gain.27 Considering reverse light propagation from the far field to generate arbitrary deep-subwavelength patterns at the bottom of the transformer, the current amount of loss could be tolerable for other applications like subwavelengt ...
... by finding low-loss negative index materials25,26 or introducing gain.27 Considering reverse light propagation from the far field to generate arbitrary deep-subwavelength patterns at the bottom of the transformer, the current amount of loss could be tolerable for other applications like subwavelengt ...
PowerPoint
... The Battle between Gravity and Pressure • Pressure pushes out and gravity pulls in– an equilibrium • This is why a main sequence star isn’t shrinking even though it’s a big ball of gas. • A star’s life is all about this ...
... The Battle between Gravity and Pressure • Pressure pushes out and gravity pulls in– an equilibrium • This is why a main sequence star isn’t shrinking even though it’s a big ball of gas. • A star’s life is all about this ...
The influence of chemical composition on the pulsation properties of
... and with different excitation potentials Accuracy 40-50 K Microturbulent velocity and gravity by minimizing the log([Fe/H]) vs. EW slope and by imposing the ionisation balance, respectively Iterative process: 5-7 iterations Sanity check with Walraven photometry (AP Pup; Pel ...
... and with different excitation potentials Accuracy 40-50 K Microturbulent velocity and gravity by minimizing the log([Fe/H]) vs. EW slope and by imposing the ionisation balance, respectively Iterative process: 5-7 iterations Sanity check with Walraven photometry (AP Pup; Pel ...
ULX accretion states
... Most ULXs dominated by p-l or Compt. component Many have soft excess + p-l + high-energy break (“ULX state”) inner disk modified by scattering-thick region at T ~ a few keV L ~ 1 – a few LEdd , M ~ 30 – 100 Msun ...
... Most ULXs dominated by p-l or Compt. component Many have soft excess + p-l + high-energy break (“ULX state”) inner disk modified by scattering-thick region at T ~ a few keV L ~ 1 – a few LEdd , M ~ 30 – 100 Msun ...
here. - SUNY Oswego
... photosphere and hydrogen ionization front (HIF). Engaged: Color of star which is related to the Temperature of photosphere = temperature of HIF. Engaged at low densities: Color of Star is related to temperature of photosphere which is less dependent on period. Engaged at high densities: more s ...
... photosphere and hydrogen ionization front (HIF). Engaged: Color of star which is related to the Temperature of photosphere = temperature of HIF. Engaged at low densities: Color of Star is related to temperature of photosphere which is less dependent on period. Engaged at high densities: more s ...
Chapter 29 Control Systems in Plants
... 2. They lack specificity 3. They act on parts of the plant other than the part that produced them. ...
... 2. They lack specificity 3. They act on parts of the plant other than the part that produced them. ...
Orion StarBlast 4.5” Telescope STAR Program
... a star slightly can help bring out its color. Deep Sky Objects: Under dark skies, you can see lots of fascinating deep sky objects, including nebulae, star clusters and a variety of different types of galaxies. Most deep sky objects are very faint, so it is important that you find an observing site ...
... a star slightly can help bring out its color. Deep Sky Objects: Under dark skies, you can see lots of fascinating deep sky objects, including nebulae, star clusters and a variety of different types of galaxies. Most deep sky objects are very faint, so it is important that you find an observing site ...
Thermal phase curves of nontransiting terrestrial exoplanets
... quantities are equal for a synchronized transiting planet with no atmosphere (for a nightside temperature of 0 K). The precision on the eclipse depth is indeed limited by the eclipse duration, which is about 9% of the orbital period. The phase- and wavelength-dependent emission of hot Jupiters has b ...
... quantities are equal for a synchronized transiting planet with no atmosphere (for a nightside temperature of 0 K). The precision on the eclipse depth is indeed limited by the eclipse duration, which is about 9% of the orbital period. The phase- and wavelength-dependent emission of hot Jupiters has b ...
Galaxy Number Counts from the Sloan Digital Sky Survey
... observations on March 20 and 21, 1999, with the telescope parked on the Celestial Equator (SDSS Runs 752 and 756). The total observation time was about seven hours in Run 752 and about eight hours in Run 756. The two runs together form a filled stripe. For r ′ < 16, we present the galaxy counts from ...
... observations on March 20 and 21, 1999, with the telescope parked on the Celestial Equator (SDSS Runs 752 and 756). The total observation time was about seven hours in Run 752 and about eight hours in Run 756. The two runs together form a filled stripe. For r ′ < 16, we present the galaxy counts from ...
SW - Calculating Magnitudes
... Background Material An object’s apparent brightness is measured in intensity or counts (depending on the software instruments that are used). In Steps 2 and 3, you should have identified that objects closer to the observer appear brighter and objects further away appear fainter. This is due to the ...
... Background Material An object’s apparent brightness is measured in intensity or counts (depending on the software instruments that are used). In Steps 2 and 3, you should have identified that objects closer to the observer appear brighter and objects further away appear fainter. This is due to the ...
Shortв•`lived radioactivity in the early solar system: The Superв•`AGB
... Soni (2006) pollution of 26Al due to the winds of lowmass AGB stars (initial masses lower than approximately 1.5 Mx) and Wolf-Rayet stars (initial masses higher than approximately 60 Mx) would have left no signature in the O isotopic composition. These two stellar sources do not produce 60Fe and to ...
... Soni (2006) pollution of 26Al due to the winds of lowmass AGB stars (initial masses lower than approximately 1.5 Mx) and Wolf-Rayet stars (initial masses higher than approximately 60 Mx) would have left no signature in the O isotopic composition. These two stellar sources do not produce 60Fe and to ...
Evolution of high-redshift quasars
... from Spitzer, which probes the hot dust heated by the AGN itself, one can then have a reliable estimate of the star formation rate in the host galaxy. ALMA, which not only has high resolution imaging in these wavelength, but also provides wealth information on various line diagnostics, will revoluti ...
... from Spitzer, which probes the hot dust heated by the AGN itself, one can then have a reliable estimate of the star formation rate in the host galaxy. ALMA, which not only has high resolution imaging in these wavelength, but also provides wealth information on various line diagnostics, will revoluti ...
Ultrahigh Precision Absolute and Relative Rotation Sensing using
... frequency, λo the vacuum wavelength of the wave and β is the boost parameter, assumed to be much less than unity for typical rotations. The form of time delay in eqn. 2 due to Sagnac effect attests to the universal fact that the time delay is simply a geometric effect, attributable to relativistic t ...
... frequency, λo the vacuum wavelength of the wave and β is the boost parameter, assumed to be much less than unity for typical rotations. The form of time delay in eqn. 2 due to Sagnac effect attests to the universal fact that the time delay is simply a geometric effect, attributable to relativistic t ...
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.