What part of the electromagnetic spectrum does the Hubble Space Telescope observe in?
The Hubble Space Telescope can view objects in more than just visible light, including ultraviolet, visible and infrared light. These observations enable astronomers to determine certain physical characteristics of objects, such as their temperature, composition and velocity.
What wavelengths of the EMS can Hubble see?
The Hubble Space Telescope is able to measure wavelengths from about 0.1150 to 2 micrometers, a range that covers more than just visible light.
Where does the Hubble telescope get its power?
Hubble is powered by solar energy, collected by the two wing-like solar arrays seen in this image of the telescope taken during the final servicing mission in 2009. One of Hubble’s original solar arrays is shown here during a deployment test, before being installed on the spacecraft.
How does the Hubble telescope use spectroscopy?
Its main function is spectroscopy-the separation of light into its component colors (or wavelengths) to reveal information about the chemical content, temperature and motion of planets, comets, stars, interstellar gas and galaxies.
How do you observe space?
ViewSpace videos tell the stories of the planets, stars, galaxies, and universe, giving viewers the opportunity to experience space and Earth as seen with satellites and telescopes. Astronomy: Explore the sky with stories told through spectacular imagery from space telescopes.
Why are dark spectral lines produced?
When light passes through gas in the atmosphere some of the light at particular wavelengths is scattered resulting in darker bands. These lines came to be known as ‘spectral lines’ and were cataloged by heating common elements until they produced light and measuring the wavelengths emitted.
Why are spectral lines not sharp?
Real spectral lines are broadened because: – Energy levels are not infinitely sharp. – Atoms are moving relative to observer. energy E of levels with finite lifetimes. Determines the natural width of a line (generally very small).
Which element has the most spectral lines?
Mercury
Why does hydrogen have so many spectral lines?
Though a hydrogen atom has only one electron, it contains a large number of shells, so when this single electron jumps from one shell to another, a photon is emitted, and the energy difference of the shells causes different wavelengths to be released… hence, mono-electronic hydrogen has many spectral lines.
Why does hydrogen only have 4 emission lines?
This is explained in the Bohr model by the realization that the electron orbits are not equally spaced. The electron energy level diagram for the hydrogen atom. He found that the four visible spectral lines corresponded to transitions from higher energy levels down to the second energy level (n = 2).
How many emission spectral lines are possible?
The number of spectral lines that are possible when electrons in the 7th shell in different hydrogen atoms return to the second shell is 15. ∴Option (B) is correct.
How spectral lines are formed?
Spectral lines are produced by transitions of electrons within atoms or ions. As the electrons move closer to or farther from the nucleus of an atom (or of an ion), energy in the form of light (or other radiation) is emitted or absorbed.…
What are the three types of spectrums?
There are three general types of spectra: continuous, emission, and absorption.
What do spectral lines tell us?
From spectral lines astronomers can determine not only the element, but the temperature and density of that element in the star. The spectral line also can tell us about any magnetic field of the star. The width of the line can tell us how fast the material is moving. We can learn about winds in stars from this.
Why do spectral lines get closer together?
The spectrum lines become closer together the further from the nucleus. This is because the energy levels are closer together further from the n energy levels they are.
Why do we see spectral lines?
The sun’s upper layers are comparatively cooler (though still very hot!), so their atoms are in lower energy states. The atoms higher in the sun absorb the light that comes up from deeper inside, thus producing the dark absorption lines we see imprinted on the solar spectrum.
How do I calculate the number of emission lines?
For example, suppose one atom with an electron at energy level 7 (n2=7). That electron can “de-excite” from n2=7 to n1=6,5,4,3,2, or 1. All those transitions give one spectral line for each. Thus, total of 1×6=n1(n2−n1) (foot note 1) spectral lines would be present in the spectrum.