TELESKOP PRESENTATION about how a teleskop astronomy work

TELESKOP ASTRONOMI, a good presentation about how to know about teleskop astronomi. This show how lens function. What is the magnified, diminished, and more important, the way we look the real image, how to clasify the virtual image. Also, you can learn about how to draw the image of teleskop astronomi, which can help you to know how to draw and learn it properly.

Here is some detail about teleskop astronomi:

Telescope astronomy is a branch of observational astronomy that uses telescopes to study celestial objects and phenomena. It allows astronomers to gather and analyze light from stars, planets, galaxies, and other cosmic structures, revealing details that are invisible to the naked eye. The development of telescopes has been instrumental in expanding our understanding of the universe, from Galileo’s first observations to modern space-based telescopes like the Hubble Space Telescope.

Telescopes come in several types, each with specific advantages and applications. The two primary categories are refracting and reflecting telescopes. Refracting telescopes use lenses to bend and focus light, while reflecting telescopes use mirrors. Reflectors, invented by Sir Isaac Newton, have largely become the preferred choice for professional astronomers due to their ability to create larger apertures without the optical distortions seen in large lenses. More advanced types, like catadioptric telescopes, combine lenses and mirrors to provide more versatility.

One of the key principles behind telescopes is the collection of light. A larger aperture, or primary mirror/lens, allows more light to be collected, resulting in a clearer and more detailed image. This capability is crucial because many astronomical objects are extremely distant and faint. Telescopes concentrate this light into an image, which can be viewed through an eyepiece or captured by sensors for further study. Modern telescopes often use digital sensors, like CCDs (charge-coupled devices), which allow for more sensitive and accurate data collection than traditional photographic methods.

Telescopes can be classified not only by their construction but also by the range of electromagnetic radiation they are designed to observe. While optical telescopes focus on the visible spectrum, radio telescopes observe longer wavelengths, revealing phenomena such as pulsars and cosmic microwave background radiation. Infrared telescopes can detect heat emitted by cooler objects like dust clouds, while X-ray and gamma-ray telescopes are used to study high-energy events like supernovae and black holes. Each type contributes to a more comprehensive picture of the universe, as different wavelengths provide different insights into the nature and behaviour of celestial objects.

One of the most significant developments in telescope astronomy is the advent of space-based telescopes. Ground-based telescopes are limited by the Earth's atmosphere, which can distort and block certain wavelengths of light Space tele

1. TELESKOP ASTRONOMI

2. CIRI IMEJ NYATA objek Imej MAYA MAYA terbentuk di sisi lain kanta bertentangan dengan objek

3. MAYA objek CIRI IMEJ NYATA imej DIPERBESAR lain terbentuk pada sisi yang sama dengan objek ,

4. DIPERBESAR CIRI IMEJ A MAYA objek imej A A

5. DIPERBESAR CIRI IMEJ A MAYA objek imej A A DIPERKECIL

6. CIRI IMEJ DIPERKECIL A DIPERBESAR A

7. CIRI IMEJ DIPERKECIL A A DIPERBESAR TEGAK

8. CIRI IMEJ TEGAK Tegak DIPERKECIL SONGSANG

9. CIRI IMEJ SONGSANG Tegak TEGAK

10. CARA LUKIS TELESKOP Fo/Fe STEP 1 U = Infiniti

11. STEP 1 U = Infiniti CARA LUKIS STEP 2 TELESKOP U = f (inverse version)

12. STEP 2 U = f (inverse version) STEP 1 STEP 3 U = Infiniti GABUNG

13. STEP 3 GABUNG STEP 2 DETAIL

14. STEP 4 DETAIL STEP 3 Fo/Fe GABUNG infiniti PELARASAN NORMAL NORMAL (demonstration)

15. PELARASAN NORMAL (demonstration) Fo/Fe infiniti STEP 4 DETAIL U = f objektif + f mata PEMBESARAN TELESKOP U f objektif f mata = M

16. PEMBESARAN TELESKOP Fo/Fe infiniti STEP 4 DETAIL U = f objektif + f mata PELARASAN NORMAL M f objektif f mata = U NORMAL (demonstration)