In this experiment setup for optical astronomy, we use high resolution telescope, digital photometer and charge-coupled devices (CCDs). Main observations are in the range of 400nm to 700 nm wavelength. The same equipment can as well be used to observe near-ultraviolet and nearinfrared radiation.
Experiments are designed for observational practice of celestial objects by using telescope and other astronomical measuring apparatus. The study of astronomy with direct experiments is not always feasible, as properties of distant universe are mostly unknown. However, this is partly compensated by the fact that astronomers have a vast number of visible examples of stellar phenomena that can be examined. This allows observational data to be plotted on graphs and general trends recorded. Nearby examples of specific phenomena, such as variable stars, can be used to infer the behavior of more distant representatives. Those distant yardsticks can then be employed to measure other phenomena in that neighborhood, including the distance to a galaxy.
Solid-state stellar photometer
A variety of data can be observed for each object. The position coordinates locate the object on the sky using the techniques of spherical astronomy, and the magnitude determines its brightness as seen from the Earth. The relative brightness in different parts of the spectrum yields information about the temperature and physics of the object. Photographs of the spectra allow the chemistry of the object to be examined.
A high resolution Solid state stellar photometer is used for the measurement of star temperature, night sky brightness, variable star study etc. It can be directly attached to the telescope. All the electronics, including detector, electrometer amplifier, voltage-to-frequency conversion electronics, and digital display are contained in one easy to handle unit. This model Stellar Photometer makes the concept of a "portable observatory" a reality. With the help of a large telescope we can make accurate and meaningful measurements of variable stars. Following experiments can be performed with HO-ED-AAP-SM02.
6.1MP 1.8" Cooled CCD camera
This experiment explores the way light is scattered by particles and shows the effect of polarization. By focusing the light to a photo detector, we can measure the polarization angle of scattered light accurately. The scattering of light by suspended molecules in water produces linearly polarized light in the plane perpendicular to the incident light. As shown in the figure, if the charges in a molecule are oscillating along the y-axis, it will not radiate along the same axis. Therefore, at 90° from the beam direction, the scattered light is linearly polarized.
Color temperature is a characteristic of visible light that has important applications in astrophysics. BV photometric technique is used to determine the temperature of an artificial star (Tungsten Halogen Lamp). BV magnitude for different voltages are taken for the experiment. Color temperature is conventionally stated in the unit of absolute temperature, the kelvin, having the unit symbol K.
Fig. Experimental setup for determination of the temperature of an artificial star by photometry.
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