Answer:
4.14 eV
Explanation:
f = 1.0 ×10^15 Hz
h= 6.63×10^-34 J s ( this is called PLANCK 'S CONSTANT)
ENEGY = E = ?
E = hf ( THIS IS FORMULA FOR ENERGY OF ONE QUANTA OR ONE PHOTON )
E= 6.63×10^-34×1.0 ×10^15
E = 6.63×10^-19 J
As 1eV = 1.6×10^-19 J so changing energy in eV from joules we will divide energy by 1.6×10^-19
hence E in eV = 6.63×10^-19/(1.6×10^-19)
E = 4.14 eV
Any substance that contains starch turns blue-black in presence of <u>iodine solution.</u>
Answer
given,
mass of satellite = 545 Kg
R = 6.4 x 10⁶ m
H = 2 x 6.4 x 10⁶ m
Mass of earth = 5.972 x 10²⁴ Kg
height above earth is equal to earth's mean radius
a) satellite's orbital velocity
centripetal force acting on satellite = 
gravitational force = 
equating both the above equation



v = 5578.5 m/s
b) 


T = 14416.92 s

T = 4 hr
c) gravitational force acting


F = 5202 N
Answer:
- Particles smaller than atoms are called subatomic particles .
- There are three famous subatomic particles, proton, neutron and electron .
- The study of sub atomic particles are called particle physics
- These particles can be divided as Brayons and Leptons
- These particles are often held together by one of the four fundamental particles ( Weak force, strong force, electromagnetic force, gravitational force).
Everything starts from spectroscopy. Astronomers only have concentrated information at wavelengths that are emitted from the stars. What they do with this information is to obtain the frequency range of the stars and through spectroscopes they are responsible for dividing the radiation beams and determining the coincidence with the emission of those same waves, of chemical elements. From these observation techniques it is possible to obtain the composition and according to the color, obtaining characteristics such as temperature. The spectrum of stars consists of dark and bright lines called Fraunhofer lines. This spectrum is compared to the spectrum of different elements to find the composition of the stars. This is possible because the elements emit or absorb only specific wavelengths.