Payal Priya
Birsa Institute of Technology (BIT), Sindri
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11 Other formulas that you can solve using the same Inputs

Distance from center to a light source for destructive interference in YDSE
Distance from center to the light source=((2*Number-1)*Wavelength*Distance between slits and screen)/(2*Distance between two coherent sources) GO
Distance from center to a light source for constructive interference in YDSE
Distance from center to the light source=(Number*Wavelength*Distance between slits and screen)/Distance between two coherent sources GO
Fringe Width
Fringe Width=(Wavelength*Distance between slits and screen)/Distance between two coherent sources GO
Optical path difference when fringe width is given
Optical path difference=(Refractive Index-1)*Thickness*Fringe Width/Wavelength GO
Distance from center to a light source for destructive interference in YDSE
Distance from center to the light source=(2*Number+1)*Wavelength/2 GO
Phase Difference
Phase Difference=(2*pi*Path Difference)/Wavelength GO
Thin-film destructive interference in reflected light
Destructive Interference=Number*Wavelength GO
Path difference for minima in Young’s double-slit experiment
Path Difference=(2*Number-1)*Wavelength/2 GO
Path difference for minima in Young’s double-slit experiment
Path Difference=(2*Number+1)*Wavelength/2 GO
Path difference of two progressive wave
Path Difference=(2*pi)/Wavelength GO
Path difference in YDSE when λ is given
Path Difference=Number*Wavelength GO

1 Other formulas that calculate the same Output

Resolving power of a microscope
Resolving power=(2*Refractive Index*sin(Theta))/Wavelength GO

Resolving power of a telescope Formula

Resolving power=Aperture of Objective/1.22*Wavelength
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Power, when electric current and resistance are given GO
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Current Density when Resistivity is Given GO
Resistivity GO
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Shear stress on circular fillet weld subjected to Torsion GO
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Focal Length Of A Concave Mirror With Virtual Image GO
Focal Length Of A Convex Mirror GO
Magnification of a Concave Mirror With Real Image GO
Magnification of a Concave Mirror With Virtual Image GO
Path difference of two progressive wave GO
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Phase Difference GO
Magnification of a Concave Mirror With Virtual Image using Height GO
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Focal length of Concave Lens GO
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Newton's law of cooling GO
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Coefficient Of Refraction Using Velocity GO
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Frequency Of Wavelength ( Using Velocity ) GO
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Angular Frequency (Using Velocity ) GO
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Angular Frequency ( Using Wave Number ) GO
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Observed Frequency When Observer Moves Away From The Source GO
Effective Wavelength When Source Moves Towards the Observer GO
Effective Wavelength When Source Moves Away From the Observer GO
Observed Frequency When Source Moves Towards the Observer GO
Observed Frequency When Source Moves Away From the Observer GO
Observed Frequency When Observer Moves Towards The Source And The Source Moves Away GO
Observed Frequency When Source Moves Towards The Observer And The Observer Moves Away GO
Observed Frequency When Observer and Source Move Towards Each Other GO
Observed Frequency When Observer and Source Move Away From Each other GO
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Frequency Of A Open Organ Pipe(4th Harmonic) GO
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Frequency Of Open Organ Pipe ( nth overtone) GO
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How is resolving power of a telescope calculated ?

In telescopes, very close objects such as binary stars or individual stars of galaxies subtend very small angles on the telescope. To resolve them we need very large apertures. We can use Rayleigh’s to determine the resolving power. R.P. = a / 1.22λ where a is the aperture of the objective and λ is the wavelength of the light used to illuminate the object.

How to Calculate Resolving power of a telescope?

Resolving power of a telescope calculator uses Resolving power=Aperture of Objective/1.22*Wavelength to calculate the Resolving power, Resolving power of a telescope is the inverse of the smallest angular separations between two distant objects, whose images are separated in the telescope. Resolving power and is denoted by RP symbol.

How to calculate Resolving power of a telescope using this online calculator? To use this online calculator for Resolving power of a telescope, enter Wavelength (λ) and Aperture of Objective (a) and hit the calculate button. Here is how the Resolving power of a telescope calculation can be explained with given input values -> 3.278689 = 2/1.22*2.

FAQ

What is Resolving power of a telescope?
Resolving power of a telescope is the inverse of the smallest angular separations between two distant objects, whose images are separated in the telescope and is represented as RP=a/1.22*λ or Resolving power=Aperture of Objective/1.22*Wavelength. Wavelength is the distance between identical points (adjacent crests) in the adjacent cycles of a waveform signal propagated in space or along a wire and Aperture of Objective is the measure of its ability to gather light and to resolve fine specimen detail while working at a fixed object distance.
How to calculate Resolving power of a telescope?
Resolving power of a telescope is the inverse of the smallest angular separations between two distant objects, whose images are separated in the telescope is calculated using Resolving power=Aperture of Objective/1.22*Wavelength. To calculate Resolving power of a telescope, you need Wavelength (λ) and Aperture of Objective (a). With our tool, you need to enter the respective value for Wavelength and Aperture of Objective and hit the calculate button. You can also select the units (if any) for Input(s) and the Output as well.
How many ways are there to calculate Resolving power?
In this formula, Resolving power uses Wavelength and Aperture of Objective. We can use 1 other way(s) to calculate the same, which is/are as follows -
  • Resolving power=(2*Refractive Index*sin(Theta))/Wavelength
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