Lecture 1
... The B ray comes to the lens moving parallel to the axis and passes through F1. The C ray which in a similar way passes through F2 and leaves the lens parallel to the optical axis. Any two of these three characteristic rays can be utilized to determine the size and placement of the image formed by th ...
... The B ray comes to the lens moving parallel to the axis and passes through F1. The C ray which in a similar way passes through F2 and leaves the lens parallel to the optical axis. Any two of these three characteristic rays can be utilized to determine the size and placement of the image formed by th ...
4.1 The Concepts of Force and Mass
... • The lens only contributes about 20-25% of the refraction, but its function is important, as it provides the fine-tuning mechanism. • The retina acts as the film, or CCD and receives the image, which it then sends, via the optic nerve, to the brain, which interprets the image. ...
... • The lens only contributes about 20-25% of the refraction, but its function is important, as it provides the fine-tuning mechanism. • The retina acts as the film, or CCD and receives the image, which it then sends, via the optic nerve, to the brain, which interprets the image. ...
CHAPTER 5 Light and Vision 2015
... The refractive index or index of refraction of a medium is equivalent to the optical density of a medium. Note: A material with greater density may not necessarily have greater optical density. The refractive index / index of refraction of a medium, n can be calculated as: n = ...
... The refractive index or index of refraction of a medium is equivalent to the optical density of a medium. Note: A material with greater density may not necessarily have greater optical density. The refractive index / index of refraction of a medium, n can be calculated as: n = ...
MACHOs
... one star so that its surface area becomes the “bullseye”. Then use the radius of the LMC to find its total area (assuming it’s a perfect circle). There are 1.9 billion starts in the LMC, multiply that by the area of one star to find the total area of bulls-eyes. Then find a ratio of bulls-eyes to th ...
... one star so that its surface area becomes the “bullseye”. Then use the radius of the LMC to find its total area (assuming it’s a perfect circle). There are 1.9 billion starts in the LMC, multiply that by the area of one star to find the total area of bulls-eyes. Then find a ratio of bulls-eyes to th ...
9. ray optics and optical instruments
... objects at all possible distances is called accommodation. 36. What is least distance of distinct vision? Write its value. The closest distance for which the eye lens can focus light on the retina is called least distance of distinct vision For normal vision it is 25 cm 37. Which are the common defe ...
... objects at all possible distances is called accommodation. 36. What is least distance of distinct vision? Write its value. The closest distance for which the eye lens can focus light on the retina is called least distance of distinct vision For normal vision it is 25 cm 37. Which are the common defe ...
ppt - University of Arizona
... years earlier (around z~10) the redshift => z~14 Epoch of first star formation - roles of NICMOS and now seem likely to have been IRAC correspond to NIRCam around z~10-15 from and MIRI on JWST. combining Spitzer and Important to note that a number of WMAP results. similar galaxies have now been fo ...
... years earlier (around z~10) the redshift => z~14 Epoch of first star formation - roles of NICMOS and now seem likely to have been IRAC correspond to NIRCam around z~10-15 from and MIRI on JWST. combining Spitzer and Important to note that a number of WMAP results. similar galaxies have now been fo ...
Doppler effect
... ω= ωobserved >ω’ = ωsource if source is approaching the observed frequency is larger than the source one and the wave length is squeezed ω= ωobserved <ω’ = ωsource if source is departing the observed frequency is smaller than the source one and the wave length is stretched (redshift) The factor γ-1 ...
... ω= ωobserved >ω’ = ωsource if source is approaching the observed frequency is larger than the source one and the wave length is squeezed ω= ωobserved <ω’ = ωsource if source is departing the observed frequency is smaller than the source one and the wave length is stretched (redshift) The factor γ-1 ...
LIGHT – REFLECTION AND REFRACTION
... which the image of an object is magnified with respect to the object size. It is expressed as the ratio of the height of the image to the height of the object. It is usually represented by the letter m. If h is the height of the object and h ′ is the height of the image, then the magnification m pro ...
... which the image of an object is magnified with respect to the object size. It is expressed as the ratio of the height of the image to the height of the object. It is usually represented by the letter m. If h is the height of the object and h ′ is the height of the image, then the magnification m pro ...
dm - The Institute of Mathematical Sciences
... cluster is formed by the collision between two galaxy clusters. While in most galaxies dark matter and visible matter are found together, in the Bullet cluster there appears to be a separation of the two. This might have happened during the collision where the stronger collisions between visible mat ...
... cluster is formed by the collision between two galaxy clusters. While in most galaxies dark matter and visible matter are found together, in the Bullet cluster there appears to be a separation of the two. This might have happened during the collision where the stronger collisions between visible mat ...
Class X Physics - Home works and Assignments Online
... 11. Does the value of speed of light change with medium? 12. What is the cause of refraction of light? 13. Which lens is used as a magnifying glass? 14. What is an optically denser medium of light? 15. What is the difference between reflection and refraction? 16. If a ray of light traveling in air i ...
... 11. Does the value of speed of light change with medium? 12. What is the cause of refraction of light? 13. Which lens is used as a magnifying glass? 14. What is an optically denser medium of light? 15. What is the difference between reflection and refraction? 16. If a ray of light traveling in air i ...
Reflection and Refraction of Light
... material is related to a quantity called the _____ __ _________, n. • Index of refraction: n=_/v – The ratio of the speed of light (_) in a vacuum to the speed of light in the medium (_). ...
... material is related to a quantity called the _____ __ _________, n. • Index of refraction: n=_/v – The ratio of the speed of light (_) in a vacuum to the speed of light in the medium (_). ...
F-stop - Edublogs
... appear to converge at that point, but they actually do not. Concave lenses have a virtual focal point. Convex lenses have a real focal point. A “virtual” image- No real image will appear on a screen. The light rays that reach your eye just behave as if they came from the image position ...
... appear to converge at that point, but they actually do not. Concave lenses have a virtual focal point. Convex lenses have a real focal point. A “virtual” image- No real image will appear on a screen. The light rays that reach your eye just behave as if they came from the image position ...
Week 9A
... which need 10 to 100 times more mass. The total needed is more than the sum of the dark matter associated with each galaxy. ...
... which need 10 to 100 times more mass. The total needed is more than the sum of the dark matter associated with each galaxy. ...
pdf format
... What Herschel Got Wrong • The star counts do indeed end at 6000light years~=2000parsecs • They are cutoff by thick clouds of dust • Dust tends to: – Absorb and scatter blue light – Has little effect on light with wavelengths longer than the size of the dust grains • The actual extent of the Milky Wa ...
... What Herschel Got Wrong • The star counts do indeed end at 6000light years~=2000parsecs • They are cutoff by thick clouds of dust • Dust tends to: – Absorb and scatter blue light – Has little effect on light with wavelengths longer than the size of the dust grains • The actual extent of the Milky Wa ...
14.5 Galactic Spiral Arms
... These objects are very close to the galactic center. The orbit on the right is the best fit; it assumes a central black hole of 3.7 million solar masses. ...
... These objects are very close to the galactic center. The orbit on the right is the best fit; it assumes a central black hole of 3.7 million solar masses. ...
Access the content
... 60. There is a relation connecting refractive indices and radii of curvature of the surfaces of a lens (a) Derive lens makers formula. [2] (b) Name the law which related to refraction. [1] 61. (a) Draw the ray diagram of a compound microscope. [2] (b) With the help of a diagram explain primary rainb ...
... 60. There is a relation connecting refractive indices and radii of curvature of the surfaces of a lens (a) Derive lens makers formula. [2] (b) Name the law which related to refraction. [1] 61. (a) Draw the ray diagram of a compound microscope. [2] (b) With the help of a diagram explain primary rainb ...
Calculation Part
... 2. A telescope has an objective lens with a focal length of 36.0 cm. The image formed by the objective lens is 0.500 cm inside the focal point of the eyepiece. Where does the image of the eyepiece appear to be if the focal length of the eyepiece is 10.00 cm? ...
... 2. A telescope has an objective lens with a focal length of 36.0 cm. The image formed by the objective lens is 0.500 cm inside the focal point of the eyepiece. Where does the image of the eyepiece appear to be if the focal length of the eyepiece is 10.00 cm? ...
file
... • OGLA and MOA alert over 1,000 new microlensing events each year primarily during the bulge season (May-September) • 12 Exoplanets have been discovered this way • Better time coverage is needed • Benefits from high resolution to reduce blending of background sources • Does not need very wide field ...
... • OGLA and MOA alert over 1,000 new microlensing events each year primarily during the bulge season (May-September) • 12 Exoplanets have been discovered this way • Better time coverage is needed • Benefits from high resolution to reduce blending of background sources • Does not need very wide field ...
Dark Matter Spiral Structure Basic Galaxy Morphology Disk Galaxy Rotation Curves:
... background star will be magnified) if the line of sight passes through the Einstein ring of one of the lenses. Previously derived the angular radius of the Einstein ring on the sky !E. Area is "!E2. ...
... background star will be magnified) if the line of sight passes through the Einstein ring of one of the lenses. Previously derived the angular radius of the Einstein ring on the sky !E. Area is "!E2. ...
24-5 Lens Concepts
... diverging lens (it diverges parallel rays away from a focal point). Like a concave mirror, converging lenses can produce a real image or a virtual image, and the image can be larger, smaller, or the same size as the object. Like a convex mirror, diverging lenses can only produce a virtual image that ...
... diverging lens (it diverges parallel rays away from a focal point). Like a concave mirror, converging lenses can produce a real image or a virtual image, and the image can be larger, smaller, or the same size as the object. Like a convex mirror, diverging lenses can only produce a virtual image that ...
Dark Matter in the Universe:
... •Jupiter-sized planets •brown dwarf stars •faint low-mass stars •black holes •white dwarf stars ...
... •Jupiter-sized planets •brown dwarf stars •faint low-mass stars •black holes •white dwarf stars ...
Debate - Studies Today
... 1) The rays of light passing parallel to the principle axis will coverage at the focus after reflection. 2) The rays of light passing through the focus will emerge parallel to the principle axis after reflection. 3) The rays of light passing through the center of curvature will all retrace their bot ...
... 1) The rays of light passing parallel to the principle axis will coverage at the focus after reflection. 2) The rays of light passing through the focus will emerge parallel to the principle axis after reflection. 3) The rays of light passing through the center of curvature will all retrace their bot ...
Answers
... A) orbits of stars, orbits of galaxies, gravitational lensing B) orbits of planets, orbits of galaxies, gravitational lensing C) orbits of planets, orbits of stars, orbits of galaxies, gravitational lensing D) orbits of planets, orbits of stars, gravitational lensing There is not enough dark matter ...
... A) orbits of stars, orbits of galaxies, gravitational lensing B) orbits of planets, orbits of galaxies, gravitational lensing C) orbits of planets, orbits of stars, orbits of galaxies, gravitational lensing D) orbits of planets, orbits of stars, gravitational lensing There is not enough dark matter ...
How can I predict how big my reflection will appear in a mirror?
... diopters, D. 1 D = 1 m-1 Optician use this notation because the total power of a set of lenses is the sum of their diopters ...
... diopters, D. 1 D = 1 m-1 Optician use this notation because the total power of a set of lenses is the sum of their diopters ...
Gravitational microlensing
Gravitational microlensing is an astronomical phenomenon due to the gravitational lens effect. It can be used to detect objects that range from the mass of a planet to the mass of a star, regardless of the light they emit. Typically, astronomers can only detect bright objects that emit much light (stars) or large objects that block background light (clouds of gas and dust). These objects make up only a tiny portion of the mass of a galaxy. Microlensing allows the study of objects that emit little or no light.When a distant star or quasar gets sufficiently aligned with a massive compact foreground object, the bending of light due to its gravitational field, as discussed by Einstein in 1915, leads to two distorted unresolved images resulting in an observable magnification. The time-scale of the transient brightening depends on the mass of the foreground object as well as on the relative proper motion between the background 'source' and the foreground 'lens' object.Since microlensing observations do not rely on radiation received from the lens object, this effect therefore allows astronomers to study massive objects no matter how faint. It is thus an ideal technique to study the galactic population of such faint or dark objects as brown dwarfs, red dwarfs, planets, white dwarfs, neutron stars, black holes, andMassive Compact Halo Objects. Moreover, the microlensing effect is wavelength-independent, allowing study of source objects that emit any kind of electromagnetic radiation.Microlensing by an isolated object was first detected in 1989. Since then, microlensing has been used to constrain the nature of the dark matter, detect extrasolar planets, study limb darkening in distant stars, constrain the binary star population, and constrain the structure of the Milky Way's disk. Microlensing has also been proposed as a means to find dark objects like brown dwarfs and black holes, study starspots, measure stellar rotation, and probe quasars including their accretion disks.