Scattering and Polarization Properties of the Scarab Beetle Cyphochilus insulanus cuticle
... studies were performed on single (5 µm thick) scales from the cuticle. Key factors for the origin of the brilliant white appearance were found to be the width (250 nm) of a non-absorbing randomly disordered internal filamentary structure and the packing density corresponding to volume occupancy of 7 ...
... studies were performed on single (5 µm thick) scales from the cuticle. Key factors for the origin of the brilliant white appearance were found to be the width (250 nm) of a non-absorbing randomly disordered internal filamentary structure and the packing density corresponding to volume occupancy of 7 ...
No Slide Title
... White Dwarfs Mass: similar to the Sun’s Diameter: about that of the Earth Hot (at least initially): 25,000 K; Dim (very small) Light they emit comes from heat (blackbody) Carbon and Oxygen; thin H/He surface layer White dwarf will cool over time (many billion of years) until it becomes a ...
... White Dwarfs Mass: similar to the Sun’s Diameter: about that of the Earth Hot (at least initially): 25,000 K; Dim (very small) Light they emit comes from heat (blackbody) Carbon and Oxygen; thin H/He surface layer White dwarf will cool over time (many billion of years) until it becomes a ...
Observation of two-photon emission from semiconductors
... GaInP/AlGaInP two-photon emission, limited only by the detector’s temporal resolution. Two-photon transitions are much weaker than the related firstorder processes, so observations of multiphoton spontaneous decays have so far been restricted to a few atomic transition cases. In these instances the ...
... GaInP/AlGaInP two-photon emission, limited only by the detector’s temporal resolution. Two-photon transitions are much weaker than the related firstorder processes, so observations of multiphoton spontaneous decays have so far been restricted to a few atomic transition cases. In these instances the ...
Atmospheric characterization of Proxima b by coupling the SPHERE
... light, Proxima b is extremely challenging to detect with SPHERE alone. The use of the high-contrast/high-resolution technique can overcome present limitations by combining a ∼103 -104 contrast enhancement from SPHERE to a ∼104 gain from ESPRESSO. Results. We find that significant but realistic upgra ...
... light, Proxima b is extremely challenging to detect with SPHERE alone. The use of the high-contrast/high-resolution technique can overcome present limitations by combining a ∼103 -104 contrast enhancement from SPHERE to a ∼104 gain from ESPRESSO. Results. We find that significant but realistic upgra ...
Filters and General Equipment for Astronomical Observing
... Although there are several astronomical suppliers that provide these filters with generic names such as Meade, Agena or Orion, all such filters are evident by their color and are usually marked with particular numbers known as Wratten numbers, which allow the observer to choose which parts of the EM ...
... Although there are several astronomical suppliers that provide these filters with generic names such as Meade, Agena or Orion, all such filters are evident by their color and are usually marked with particular numbers known as Wratten numbers, which allow the observer to choose which parts of the EM ...
Magnetic fields in Local Group dwarf irregulars⋆
... et al. 2008). Although dSphs experienced star formation over extended time intervals in their youth, today all of them but one appear to be completely free of detectable interstellar material (Grebel et al. 2003). A new population of ultrafaint dSphs (UF dSphs) with absolute magnitude MV ≥ −6 were o ...
... et al. 2008). Although dSphs experienced star formation over extended time intervals in their youth, today all of them but one appear to be completely free of detectable interstellar material (Grebel et al. 2003). A new population of ultrafaint dSphs (UF dSphs) with absolute magnitude MV ≥ −6 were o ...
Which part of the spectrum can be separated into
... 1. Which part of the spectrum can be separated into rainbow like colors? Answer: visible light 2. Which waves have the shortest wave lengths? Longest? Answer: gamma; radio 3. What is a spectroscope/prism used for? Answer: split white light into colors 4. What kind spectrum is used to determine the c ...
... 1. Which part of the spectrum can be separated into rainbow like colors? Answer: visible light 2. Which waves have the shortest wave lengths? Longest? Answer: gamma; radio 3. What is a spectroscope/prism used for? Answer: split white light into colors 4. What kind spectrum is used to determine the c ...
Process of Science: PreMainSequence Stellar Life Tracks on the HR
... 2. All the stars in the cluster formed from the same interstellar cloud and therefore began to form at about the same time. Astronomers can therefore use star clusters as laboratories for comparing the properties of stars at about the same distance or of about the same age. ANSWER: By observing and ...
... 2. All the stars in the cluster formed from the same interstellar cloud and therefore began to form at about the same time. Astronomers can therefore use star clusters as laboratories for comparing the properties of stars at about the same distance or of about the same age. ANSWER: By observing and ...
lecture 3 Introduction to Laser
... Mode-locking is a technique in by which a laser can be made to produce pulses of light of extremely short duration, on the order of picoseconds (10−12s) or femtoseconds (10−15s). Need for Mode Locking When laser is oscillating with various modes and if modes are uncorrelated The output intensity i.e ...
... Mode-locking is a technique in by which a laser can be made to produce pulses of light of extremely short duration, on the order of picoseconds (10−12s) or femtoseconds (10−15s). Need for Mode Locking When laser is oscillating with various modes and if modes are uncorrelated The output intensity i.e ...
Physics 41N Lecture 2: Dimensional Analysis
... gazelles to giraffes. The top speed was basically constant, decreasing slightly in the larger animals. ...
... gazelles to giraffes. The top speed was basically constant, decreasing slightly in the larger animals. ...
Low-dispersion Spectroscopy
... ΔR(λ) = R(λ) – R(5000Å) ~ cste [n(λ) – n(5000)] tan z Ex: for AM = 1.5, λ=4000 Å, ΔR ~ 0.70’’ : relative loss of flux Depends on P and T (altitude) and humidity Worse in the blue, negligible in the near-IR • Use parallactic angle for slit (oriented along the refraction) ...
... ΔR(λ) = R(λ) – R(5000Å) ~ cste [n(λ) – n(5000)] tan z Ex: for AM = 1.5, λ=4000 Å, ΔR ~ 0.70’’ : relative loss of flux Depends on P and T (altitude) and humidity Worse in the blue, negligible in the near-IR • Use parallactic angle for slit (oriented along the refraction) ...
Self-Regulation of Star Formation in Low Metallicity Clouds
... After the recombination era, little information is accessible until z ∼ 5, after that we can observe objects such as galaxies and QSOs. On the other hand, the reionization of the intergalactic medium and the presence of heavy elements at high-z suggest that there are other populations of luminous ob ...
... After the recombination era, little information is accessible until z ∼ 5, after that we can observe objects such as galaxies and QSOs. On the other hand, the reionization of the intergalactic medium and the presence of heavy elements at high-z suggest that there are other populations of luminous ob ...
Controlling light-with-light without nonlinearity
... patterning, one can manipulate the balance among absorption, transmission and reflection in sub-wavelength plasmonic films to achieve desired levels at any visible/infrared wavelength. Figure 3c shows modulation of total output intensity resulting from modulation of control intensity in the time dom ...
... patterning, one can manipulate the balance among absorption, transmission and reflection in sub-wavelength plasmonic films to achieve desired levels at any visible/infrared wavelength. Figure 3c shows modulation of total output intensity resulting from modulation of control intensity in the time dom ...
MICROWAVE AND LIGHT INTERFERENCE - Galileo
... the intensity of the electromagnetic waves at any point, we must first add up (as vectors, of course), all of the electric fields to find the net electric field. We cannot simply add intensities. It is this property of electromagnetic waves1 that lead to interference effects. In this workshop you wi ...
... the intensity of the electromagnetic waves at any point, we must first add up (as vectors, of course), all of the electric fields to find the net electric field. We cannot simply add intensities. It is this property of electromagnetic waves1 that lead to interference effects. In this workshop you wi ...
WHITE DWARFS AS A SOURCE OF CONSTRAINTS ON EXOTIC …
... White dwarfs are degenerate stars , consist of C and O, they could also have thin outher He and H layers. ...
... White dwarfs are degenerate stars , consist of C and O, they could also have thin outher He and H layers. ...
Optical Instruments
... The solid B whose refractive index is to be determined is taken having two faces cut perpendicular to one another. The faces are made perfectly plane. The solid B is placed on the prism A. To bring perfect contact between the horizontal faces of A and B, a few drops of a liquiq whose refractive inde ...
... The solid B whose refractive index is to be determined is taken having two faces cut perpendicular to one another. The faces are made perfectly plane. The solid B is placed on the prism A. To bring perfect contact between the horizontal faces of A and B, a few drops of a liquiq whose refractive inde ...
Fano resonances in the excitation spectra of semiconductor
... spectra in the presence of a magnetic field applied perpendicularly to the layers. Modification of the PLE spectrum became noticeable at a magnetic field exceeding 0.5 T. The oscillator strength of the 1s-lh exciton is gradually reduced in favor of excited excitonic states with higher quantum number ...
... spectra in the presence of a magnetic field applied perpendicularly to the layers. Modification of the PLE spectrum became noticeable at a magnetic field exceeding 0.5 T. The oscillator strength of the 1s-lh exciton is gradually reduced in favor of excited excitonic states with higher quantum number ...
White dwarf cooling sequences and cosmochronology
... uniformity of the models with log(L/L ) ≤ −1.5. Furthermore, since the time necessary to reach this value is ≤ 8 × 107 years for any model, its influence in the total cooling time is negligible [19], except of course at large luminosities. Fluid cooling: This phase occurs at luminosities −1.5 ≥ log ...
... uniformity of the models with log(L/L ) ≤ −1.5. Furthermore, since the time necessary to reach this value is ≤ 8 × 107 years for any model, its influence in the total cooling time is negligible [19], except of course at large luminosities. Fluid cooling: This phase occurs at luminosities −1.5 ≥ log ...
arXiv:astro-ph/0701792v1 29 Jan 2007
... dynamical time, so the star formation feedback should be stronger there than in the outer region. The total net star-forming feedback is outward at large scale (however, we must bear in mind that it may not be the case at very small scale, see discussions in §4), and the outward star-forming feedbac ...
... dynamical time, so the star formation feedback should be stronger there than in the outer region. The total net star-forming feedback is outward at large scale (however, we must bear in mind that it may not be the case at very small scale, see discussions in §4), and the outward star-forming feedbac ...
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.