How to find magnificationof a lens

A practical example: if you are using a telescope with 200 mm lens aperture, the minimum useful magnification is around 28 times. If the telescope aperture was larger, the minimum magnification must be higher. For a smaller telescope, it is correspondingly smaller.

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It is used to convert linear polarization into circular polarization, but also commonly used for the polarization measurements.

A quantum cascade laser (QCL) is a semiconductor laser that emits in the mid- to far-infrared region of the electromagnetic spectrum.

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Strobe lights (or stroboscopes) have been used to study rotating machinery, oscillating vibrations and rotational speeds for balancing.

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A telescope creates a focal point, depending on the curvature of the mirrors or lenses. With the focal length alone, a small level of magnification will be achieved. But in order to be able to look at the image, you additionally need an eyepiece. Imagine an eyepiece as a magnifying glass which enlarges the image at the focal point.

A half waveplate is used when aligning P and S-polarized light which is separated by PBS into same polarization direction. Below is an example of optical system to expose the grating by two-beam interferometry. Interference fringes with good contrast can be obtained by aligning the polarization direction.

Minimum magnification is limited by the telescope’s aperture. Here, the exit pupil should not be larger than seven millimetres. This is usually also the maximum diameter that the pupil of the human eye can reach. But this is only possible at night and in absolute darkness.

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The half waveplate is used to change direction of the linear polarization. When the crystal axis (fast axis or slow axis) is aligned parallel with the polarization direction of the incident beam, the polarization of the exit beam will maintain the same direction. When the crystal axis of the waveplate is rotated for θ from polarization direction of the incident beam, the polarization of the exit beam rotates for 2θ from polarization direction of the incident beam. Using this effect, the direction of the linear polarization is arbitrarily rotated with the rotation of the half waveplate. This method has a merit that the polarization direction is rotatable without change in light intensity. When the polarization direction of the waveplate is rotated for 90°, the extinction ratio of linear polarization is slightly deteriorated due to the retardation error. For this reason, insertion of a polarizer next to the waveplate is recommended for the precise polarization measurement, which requires high extinction ratio. If a quartz waveplate with high parallelism is used, the polarization direction can be changed without beam deflection.

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In experiments using a laser, the laser oscillation may be unstable if the back reflection from mirror or optics is returned to the laser. An optical isolator is used to prevent this returning light. A typical optical isolators are composed of quarter waveplate and a polarizer. The light passes through the quarter waveplate two times during the round-trip reflection. Since the circular polarization does not change its rotational direction in mirror reflection, the retardation of total 180 degrees is obtained from phase difference amount of twice passed through the quarter waveplate. With the retardation obtained, the polarization direction of the mirror reflection, which passes the quarter waveplate is rotated by 90 degrees with respect to the incident polarization direction. This will make reflected light not able to pass through the polarizer, and block out the back reflection.

Maximum useful magnification is reached with an eyepiece exit pupil of 0.7 mm - 0.8 mm. It is not a precisely defined limit, more a guide for optimum magnification.

Feature of quarter wave plates is that it is possible to convert incident linear polarization into circular polarization, but also into other state of linear polarization or various elliptical polarization. Conversely, when elliptical axis of incident light is accurately aligned against quarter waveplate optical axis, arbitrary elliptical polarization can be converted into linear polarization. The azimuth γ of the incident linear polarization is defined by the ellipticity of the elliptical polarization, which corresponds to half of the retardation Δ. The polarization measurement using this principle is named Senarmont method. Senarmont method is commonly used when measuring minute stress (birefringence).

For example, if you have a telescope with a focal length of 1,000 mm and an eyepiece with a focal length of 5 mm, you'll get 200 times magnification.

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More magnification equals a better telescope? Beginners often think this, but it is not the determining factor, small or medium levels of magnification are usually more effective. Here you can learn how to calculate magnifications.

Each telescope has its own magnification limit. It is equivalent to 2 times the lens aperture. However, you cannot and should not use this upper limit every night. This is because you will only enjoy observing if the object is bright enough and the seeing is perfect. It is easy to find out for yourself whether it makes sense to operate at this limit: use an eyepiece with a 0.5mm exit pupil and pay attention to the seeing. How does the object appear? Is it blurred? Is it too dark? How are the conditions tonight?

A telescope with an aperture of 100 mm would therefore have a optimum magnification of 142-times and a 200 mm telescope of 285-times.

Unfortunately, no telescope nor any other optical instrument is completely defect-free. Here we describe the most important image defects found in astronomical telescopes.

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Magnification depends on the ratio of the telescope's focal length to the focal length of the eyepiece. To calculate this, divide the focal length of the telescope (ft) by the focal length of the eyepiece (fe):

Divide the telescope's aperture by the diameter of the maximum aperture of the eye’s pupil, to get the minimum useful magnification.

In theory, magnification is unlimited. However, since it is related to the aperture of the optics, there are limits. The exit pupil also plays an important role. This is the diameter of the beam of light that leaves the eyepiece and enters the eye. We’ll come to this again later.

Optimum magnification or maximum useful magnification is reached when a star no longer appears point-shaped, but as a tiny disk with diffraction rings. At this point, you are using all the optics’ available resolving power. This means that you can see many details that remain hidden at a lower or higher magnifications.

How to find magnificationin physics

The wave plate can manipulate the polarization state without a change in light intensity. Commonly used applications for the λ/2 and λ/4 Wave plate are described in Singapore.

By combining the polarization beam splitter (PBS) and half waveplate, it is possible to vary the light intensity. The method can be used to adjust the reflectance as well as the transmittance, and also for ratio between transmission and reflection. This method is highly efficient, which transmittance loss is all converted into the reflectance gain. One of the features is dynamic range of light intensity adjustment. (97% to 0.3%, depending on the quality of the PBS)

There are three important magnifications that every amateur astronomer can easily determine. Here we show you how you do this.

A Michelson interferometer using a PBS and quarter waveplates is introduced. Utilizing the polarization, the unnecessary back reflection is reduced and stability of the interference fringes is enhanced. Incident light is collected on the observation side without a loss, but in order to observe polarization, insertion of the polarizer is demanded with 50% reduction of light intensity.

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The situation is significantly different for infinity-corrected optical systems where the objective produces a flux of parallel light wavefronts imaged at ...