Which of the following can be determined by looking at the spectrum of a star?

Which of the following can be determined by looking at the spectrum of a star?

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.

Which of the following can be determined from the spectrum of a star quizlet?

Spectroscopy of a star can reveal its temperature, composition, and line-of-sight motion.

What property of a star does its spectrum class directly indicate?

-The spectral type of a star uniquely determines its color. The spectral type of a star is directly related to its color.

What information can we learn about a star from a single spectrum select all answers that apply?

Analyzing the spectrum of a star can teach us all kinds of things in addition to its temperature. We can measure its detailed chemical composition as well as the pressure in its atmosphere. From the pressure, we get clues about its size. We can also measure its motion toward or away from us and estimate its rotation.

Which of the following can be determined by using the Doppler effect?

Which of the following can be determined by using the Doppler effect? The speed at which a star is moving away from an observer, the radial velocity of a star, and the speed at which a car is traveling towards an observer.

Which of the following telescopes is or will be best suited for studying the hottest?

What observations characterize solar maximum? There are many sunspots visible on the surface of the sun. How much does the Sun lose through nuclear fusion per second? What is the only force that can overcome the repulsion between two positively charged nuclei and bind them together?

What is the most important criteria to classify spectral types of star?

The modern spectral classification system is so successful that it has hardly been changed since 1943. It is based on just two physical properties that imprint themselves on the spectrum of a star’s light: the star’s surface temperature and atmospheric pressure.

How is spectral class determined?

The spectral class of a star is a short code primarily summarizing the ionization state, giving an objective measure of the photosphere’s temperature. This is based on the width of certain absorption lines in the star’s spectrum, which vary with the density of the atmosphere and so distinguish giant stars from dwarfs.

What are three properties of stars that could be determined from its spectrum?

Apart from these three, the spectrum can be used to help determine:

• Density.
• Mass.
• Distance.
• Luminosity.

How is the wavelength of a star determined?

The spectrum of the star is is used to study its composition, motion and surface temperature. The absorbed or emitted wavelength indicates the elements present. The peak wavelength determines the surface temperature of the star using Wein’s law. Peak wavelength is inversely proportional to temperature.

How does the spectra of a star work?

A star’s spectrum contains information about its temperature, chemical composition, and intrinsic luminosity. Spectrograms secured with a slit spectrograph consist of a sequence of images of the slit in the light of the star at successive wavelengths.

How does density affect the spectral lines of a star?

This effect is due to collisions between particles in the star’s photosphere—more collisions lead to broader spectral lines. Collisions will, of course, be more frequent in a higher-density environment. Think about it like traffic—collisions are much more likely during rush hour, when the density of cars is high.

What are the spectral lines of a giant star?

A giant star with a very-low-pressure photosphere shows very narrow spectral lines (bottom), whereas a smaller star with a higher-pressure photosphere shows much broader spectral lines (top). (credit: modification of work by NASA, ESA, A. Field, and J. Kalirai (STScI))