Models of the Structure and Evolution of Protoplanetary Disks
... The energetic domain of its SED therefore has a slope of νFν ∝ νs with s = 4/3 = 1.33, which follows from the fact that any disk with Teff ∝ r –q has an SED slope of s = (4q – 2)/q. This steep slope arises because most of the stellar radiation is absorbed and reemitted at small radii where the disk ...
... The energetic domain of its SED therefore has a slope of νFν ∝ νs with s = 4/3 = 1.33, which follows from the fact that any disk with Teff ∝ r –q has an SED slope of s = (4q – 2)/q. This steep slope arises because most of the stellar radiation is absorbed and reemitted at small radii where the disk ...
Observed emission rates in sprite streamer heads
... which is controlled externally by the user. The calibration constant C can then be determined through analysis of the star field. C reflects optical and electronic gains, which we assume to be wavelength independent. [13] The star spectra P(l) were derived from the ‘‘Thirteen-Color Photometry of 138 ...
... which is controlled externally by the user. The calibration constant C can then be determined through analysis of the star field. C reflects optical and electronic gains, which we assume to be wavelength independent. [13] The star spectra P(l) were derived from the ‘‘Thirteen-Color Photometry of 138 ...
space – journey across the solar system
... Cut lengths of string/wool into 30cms. Tie the lengths of string/wool to the long piece of string so that they are evenly space along its length but making sure that there is enough room at each end for a leader to hold onto. Tie the other end of each short length with a burger ring or cheezel. Cont ...
... Cut lengths of string/wool into 30cms. Tie the lengths of string/wool to the long piece of string so that they are evenly space along its length but making sure that there is enough room at each end for a leader to hold onto. Tie the other end of each short length with a burger ring or cheezel. Cont ...
The dynamical lives of high redshift galaxies - dragons
... short time between minor mergers. We illustrate this by using standard relaxation metrics to establish two dynamical recovery timescales: halos need two dynamical times since formation (τform >2) and three dynamical times since a major (3:1) or minor (10:1) merger (τmerge >3) to be relaxed. The reco ...
... short time between minor mergers. We illustrate this by using standard relaxation metrics to establish two dynamical recovery timescales: halos need two dynamical times since formation (τform >2) and three dynamical times since a major (3:1) or minor (10:1) merger (τmerge >3) to be relaxed. The reco ...
Design and construction of a refracting telescope
... spectrum creating a magnified image for direct view. view The optical telescope uses optical components like mirrors, lenses and solid state detectors to observe light lig from the near infrared to the near ultra-violet ultra wavelengths. From the electromagnetic spectrum, wavelengths of approximate ...
... spectrum creating a magnified image for direct view. view The optical telescope uses optical components like mirrors, lenses and solid state detectors to observe light lig from the near infrared to the near ultra-violet ultra wavelengths. From the electromagnetic spectrum, wavelengths of approximate ...
The similarity of the stellar mass fractions of galaxy groups and
... studies mentioned above inferred the total stellar mass by applying a simple stellar M/L ratio conversion. L12 argue that applying a single conversion factor to all galaxies will bias the estimate of fstar , since not all galaxies in groups and clusters are quiescent and furthermore the fraction of ...
... studies mentioned above inferred the total stellar mass by applying a simple stellar M/L ratio conversion. L12 argue that applying a single conversion factor to all galaxies will bias the estimate of fstar , since not all galaxies in groups and clusters are quiescent and furthermore the fraction of ...
Theoretical criteria for scattering dark states in nanostructured particles Chia Wei Hsu,
... Consider a linearly polarized planewave incident on an obstacle that is spherical or nonspherical but much smaller than the wavelength of the incident light. This obstacle can have arbitrary number of layers and material composition; in the small-obstacle case, it can also be a cluster of particles. ...
... Consider a linearly polarized planewave incident on an obstacle that is spherical or nonspherical but much smaller than the wavelength of the incident light. This obstacle can have arbitrary number of layers and material composition; in the small-obstacle case, it can also be a cluster of particles. ...
Post-Common-Envelope Binaries from the Sloan Digital Sky Survey
... I deeply thank Dr. Boris Gänsicke for his excellent guidance through my PhD, for his help and suggestions, and most importantly for making it possible for me to develop my qualities as a researcher. I am also deeply thankful for his trust in me in this and other projects. Without him this thesis wo ...
... I deeply thank Dr. Boris Gänsicke for his excellent guidance through my PhD, for his help and suggestions, and most importantly for making it possible for me to develop my qualities as a researcher. I am also deeply thankful for his trust in me in this and other projects. Without him this thesis wo ...
View/Open - NUI Galway
... implement, and if the signals of interest tend to fluctuate slowly very sensitive measurements can be made. For these reasons, DOTP imaging polarimeters are the preferred solution for current very large and future extremely large telescopes such as SPHERE-ZIMPOL on the VLT (Roelfsema et al 2011). Di ...
... implement, and if the signals of interest tend to fluctuate slowly very sensitive measurements can be made. For these reasons, DOTP imaging polarimeters are the preferred solution for current very large and future extremely large telescopes such as SPHERE-ZIMPOL on the VLT (Roelfsema et al 2011). Di ...
Andrea Santangelo
... • How the energy of the line is related to the luminosity ? Do we observe a change of regime ...
... • How the energy of the line is related to the luminosity ? Do we observe a change of regime ...
final repor - Faculty Server Contact
... proprietary skin preparation system to improve the accuracy of the reverse iontophoresis technique. The skin preparation system, Prelude, is a tool which uses electricity and feedback algorithms to painlessly remove the top layer of skin. This layer is mainly comprised of dead skin cells and has bee ...
... proprietary skin preparation system to improve the accuracy of the reverse iontophoresis technique. The skin preparation system, Prelude, is a tool which uses electricity and feedback algorithms to painlessly remove the top layer of skin. This layer is mainly comprised of dead skin cells and has bee ...
8 Comets: Potential Sources of Prebiotic Molecules for the
... The expansion speed of most molecules in the coma is about 1 km/s. Photodissociation reactions take place, for example H2 O → H + OH, followed by OH → O + H. For the photodissociation fragments, the speeds can reach several km/s (8 and 21 km/s in the case of H produced from H2 O). The matter ejected ...
... The expansion speed of most molecules in the coma is about 1 km/s. Photodissociation reactions take place, for example H2 O → H + OH, followed by OH → O + H. For the photodissociation fragments, the speeds can reach several km/s (8 and 21 km/s in the case of H produced from H2 O). The matter ejected ...
FABRY PEROT RESONATOR
... k(xR-xM)is the phase shifting of the measurement wave as opposed to the reference wave, which occurs because the path of the measuring beam through the index arm of the interferometer is longer or shorter than the path of the reference arm. This phase shifting is also known as the path difference an ...
... k(xR-xM)is the phase shifting of the measurement wave as opposed to the reference wave, which occurs because the path of the measuring beam through the index arm of the interferometer is longer or shorter than the path of the reference arm. This phase shifting is also known as the path difference an ...
Characterizing filaments in regions of high-mass star
... steps in the star formation process. The observations support a picture of low-mass star formation according to which ∼ 0.1 pc-wide filaments form first in the cold interstellar medium, probably as a result of large-scale compression of interstellar matter by supersonic turbulent flows, and then pre ...
... steps in the star formation process. The observations support a picture of low-mass star formation according to which ∼ 0.1 pc-wide filaments form first in the cold interstellar medium, probably as a result of large-scale compression of interstellar matter by supersonic turbulent flows, and then pre ...
Other Worlds: Analyzing the Light Curves of
... source star (Beaulieu et al. 2006). This is useful since this is exactly the range within which radial velocity measurements and transit light curves are not very sensitive, and it covers a range of size and orbital distances that could include an Earth-sized planet in the habitable zone (Bennett & ...
... source star (Beaulieu et al. 2006). This is useful since this is exactly the range within which radial velocity measurements and transit light curves are not very sensitive, and it covers a range of size and orbital distances that could include an Earth-sized planet in the habitable zone (Bennett & ...
Editable Schemes of Work - Approach 1
... Practical support to help you deliver this Edexcel specification Scheme of work This scheme of work has been produced to help you implement this Edexcel specification. It is offered as an example of one possible model that you should feel free to adapt to meet your needs and is not intended to be i ...
... Practical support to help you deliver this Edexcel specification Scheme of work This scheme of work has been produced to help you implement this Edexcel specification. It is offered as an example of one possible model that you should feel free to adapt to meet your needs and is not intended to be i ...
Evolution and fate of very massive stars
... et al. (2001), which compare rather well with observations (Crowther et al. 2010; Muijres et al. 2011). For stars in a domain not covered by the Vink et al prescription, we applied the de Jager et al. (1988) prescription to models with log(Teff ) > 3.7. For log(Teff ) 6 3.7, we performed a linear fi ...
... et al. (2001), which compare rather well with observations (Crowther et al. 2010; Muijres et al. 2011). For stars in a domain not covered by the Vink et al prescription, we applied the de Jager et al. (1988) prescription to models with log(Teff ) > 3.7. For log(Teff ) 6 3.7, we performed a linear fi ...
Full text - UvA/FNWI - University of Amsterdam
... with optical lattices have been proposed as possible setups to do quantum information processing [ ]. The aim of the project for this thesis was to build the experimental setup for the optical lattice and implement it on the Celsius experiment. The next goal was to characterize the setup and show th ...
... with optical lattices have been proposed as possible setups to do quantum information processing [ ]. The aim of the project for this thesis was to build the experimental setup for the optical lattice and implement it on the Celsius experiment. The next goal was to characterize the setup and show th ...
YEAR - University of Maryland Astronomy
... Monsters in the Sky: Quasars and Supermassive Black Holes How to Make Asteroid Families and Satellites Binary Black Holes Space Weather Bars in Near by Spiral Galaxies Not Stars The Sun's Magnetic Field How Stars Form X-Rays and Gamma Rays on the Sun The Problem with Mars Fasten Your Seatbelts! The ...
... Monsters in the Sky: Quasars and Supermassive Black Holes How to Make Asteroid Families and Satellites Binary Black Holes Space Weather Bars in Near by Spiral Galaxies Not Stars The Sun's Magnetic Field How Stars Form X-Rays and Gamma Rays on the Sun The Problem with Mars Fasten Your Seatbelts! The ...
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.