Best writers. Best papers. Let professionals take care of your academic papers

Order a similar paper and get 15% discount on your first order with us
Use the following coupon "FIRST15"
ORDER NOW

What is a Balmer transition in a hydrogen molecule? What

/in /by

Get college assignment help at Smashing Essays Question

  • What is a Balmer transition in a hydrogen molecule? What type of photon will be released? Explain how the phrase “all laws of physics are the same everywhere in the Universe” applies to the analysis of this process.

Seismic Waves and The interior of the Moon

Write a one page paper over the following question.The analysis of seismic waves helped scientists determine that the Earth’s inner core is solid and the outer core is molten. Could the same technology be used to learn about the interior of the Moon?

Astronomy Question Write an essay in which you describe how astronomers have used powerful

Write an essay in which you describe how astronomers have used powerful telescopes to make important discoveries in astronomy, and how these discoveries have changed our understanding of the universe. Be sure to include at least two important discoveries, an explanation of how these discoveries have changed our understanding of the universe, and examples of the instruments, such as telescopes, used to make these discoveries. Support your discussion with evidence from the reading and Dark Universe.

he Doppler shift is used to findQuestion 11 options:eclipsing binaries.spectroscopic

Question he Doppler shift is used to findQuestion 11 options:eclipsing binaries.spectroscopic binaries.visual binaries.astrometric binaries.photometric binaries.Question 12 (4 points)A certain star has an apparent magnitude of 3 and an absolute magnitude of -1. How far away is this star?Question 12 options:10 pc awaymore than 10 pc awayless than 10 pc awayWe would need to know the star’s spectral type to find its distancQuestion 17 (4 points)What product of the fusion reaction occurring in the core of the Sun is directly observable?Question 17 options:heliumpositronsphotonsneutrinos

During a period of high solar activity, the coronaQuestion 24

Question During a period of high solar activity, the coronaQuestion 24 options:disappears.is more irregular.cools almost to the temperature of the photosphere.becomes smooth and even.shrinks to half its normal size.Question 21 (4 points)SavedSunspotsQuestion 21 options:are always found close to the Sun’s poles.come in pairs, representing the north and south magnetic fields.were most numerous during the Maunder Minimum.travel over the surface of the Sun from pole to pole.are relatively constant in number every year.

Briefly describe what the HR diagram is, and why it

Question Briefly describe what the HR diagram is, and why it is important for our understanding of stars.

How does the Sun produce the energy required to keep

Question How does the Sun produce the energy required to keep its internal temperature high enough for gas pressure to counteract the inward pull of gravity?

Physics Help please answer all. 1)A 2190 KG space station

Question Physics Help please answer all. 1)A 2190 KG space station orbits Earth at an altitude of 5.49 x 10^5. Find the magnitude of the force with which the station attracts earth. The mass and mean radius of Earth are 5.98 X 10^24 kg and 6.37 X 10^6 m, respectively. What is the force? 2)During a solar eclipse, the Moon is positioned directly between Earth and the sun. Find he magnitude of the net gravitational force acting on the Moon during the Solar eclipse due to both Earth and the Sun. The masses of the Sun, Earth, and the Moon at 1.99X10^30 kg, 5.98X10^24 kg, and 7.36 X 10^22 kg, respectively. The Moons mean distance from Earth is 3.84 X 10^8 m, and a earth’s mean distance from the sun is 1.50 C 10^11 m. The gravitational constant is G= 6.67 X 10^ -11 Nm^2/KG^2. What is the magnitude of net gravitational force on the Moon? 3)Assuming that the earth has a uniform density p=5540.0 kg/m^3 what is the value of the gravitational acceleration at a distance d=3600.0 km from the earths center?4)One of your summer lunar space camp activities is to launch a 1130 kg rocket from the surface of the moon. You are a serious space camper and you launch a serious rocket: it reaches and altitude of 215km. What gain in gravational potential energy does the launch accomplish? The mass and radius of the Moon are 7.36 X 10^22 kg and 2740 km, respectively. What is the gravitational potential energy in J? 5)Astromers discover an exoplanet that has an orbital period of 3.01 Earth years in its circular orbit around its sun, which is a star with a measured mass of 3.51X10^30 kg. Find the radius of the exoplanets orbit. What is the radius in M?6)A planet of mass m= 4.95X10^24 kg is orbiting in a circular path a star of mass M=5.05X10^29kg. The radius of the orbit R=7.45X10^7 km. What is the orbital period in Earth days of the planet T? 7)A team of astronauts is on a mission to land on and explore a large asteroid. In addition to collecting samples and performing experiments, one of their tasks is to demonstrate the concept of the escape speed by throwing rocks straight up at various initial speeds. With what minimum initial speed Vsec will the rocks need to be thrown in order for them to never fall back to the asteroid? Assume that the asteroid is approximately spherical, with an average density P=2.80X10^6 g/m^3 and volume V=2.86X10^13 m^3. Recall that the universal gravitational constant is G=6.67X10^-11 N•m^2 /KG^2. What is the Vsec in m/s? 8)An asteroid is discovered in a nearly circular orbit around the sun, with an orbital radius that is 3.93 times Earths. What is the asteroids orbital period T, it’s year in terms of Earths years? T= ____years? 9)The schwarzschild radius is the distance from an object at which the escape velocity is equal to the speed of light. A black hole is an object that is smaller than its Schwarzschild radius, so not even light itself can escape a black hole. The schearzschild radius r depends on the mass m of the black hole according to the equation. R=2Gm/c^2Where G=6.673X10^-11 N•m^2 / Kg^2 is the gravitational constant and c=2.998X10^8 m/s is the speed of light. -Consider a black hole with a mass of 1.90X10^7 M. Use the given equation to find the Schwarzschild radius for this black hole. -What is the radius in units of the solar radius? 

The ultimate fate of the Sun: in a paragraph describe

Question  The ultimate fate of the Sun: in a paragraph describe what a white dwarf is, its origins, its physical characteristics, what physical processes are important for it, and its ultimate fate.

Assuming Mars is in radiative equilibrium calculate its temperature K

Question Assuming Mars is in radiative equilibrium calculate its temperature K using the appropriate equation

What is the difference between the recently famous pictured black

Get college assignment help at Smashing Essays Question What is the difference between the recently famous pictured black hole and the one that style=”color:rgb(45,59,69);”> Betelgeuse will leave (may already have left) behind?Have we definitely demonstrated black holes exist?

No idea how to answer this, I do not see

Question No idea how to answer this, I do not see any lines on the Sun pic.. alt=”Spectrum_of_Light_Question_16.png” /> ATTACHMENT PREVIEW Download attachment Spectrum_of_Light_Question_16.png Our Sun like all stars, has absorption lines in its spectrum. The great heat of the Sun produces a continuous spectrum, and then the cooler, thin gasses at the outer edge of the Sun absorb some of the wavelengths from the spectrum. By identifying the lines in the spectrum we can learn about what gasses are present in the Sun. The spectrometer in your kit is not sensitive enough to let you see the lines so I am providing photos below. The top image of the Sun’s spectrum came from a site posted by Rob Brown. http://home.comcast.net/~mcculloch-brown/astro/spectrostar.html The arrows show some (not all) of the absorption lines. 1.8 1,9 , 20 22. 24 26 2.8 30 32 34 The Sun 700 – 600 500 400 Hydrogen Gas Helium Gas Neon Gas Analyze the four images. Try to match the lines from the spectra of the different gasses to the absorption lines in the Sun. Which, if any, of the three gasses can be found in the Sun? Tell me which lines you can match up and what gasses they belong to. If a particular element is present in the Sun’s spectrum you should be able to find all of the lines of that spectrum. For instance, if there is hydrogen in the Sun you should find a dark line in the red below 650 nm, a dark line in the blue- green at about 485 nm and a dark line in the blue near 430 nm. If you find only one or two of the lines and not the whole pattern then probably the lines are from some other element. There are a lot of points in this question so do a careful job with your answer. In the past students have been lazier than I would like with this question. Show them up. Go through line by line and tell me which lines you see. Don’t limit yourself to the ones I marked with arrows. Those were done just to make it clear what I was talking about.

Spectrum of Stars – Q1Background info src=”/qa/attachment/8320033/” alt=”Spectrum_of_Stars_Back_ground_info_1.png” />Question: Attachment

Question Spectrum of Stars – Q1Background info src=”/qa/attachment/8320033/” alt=”Spectrum_of_Stars_Back_ground_info_1.png” />Question: Attachment 1 Attachment 2 Attachment 3 Attachment 4 ATTACHMENT PREVIEW Download attachment Spectrum_of_Stars_Back_ground_info_1.png Stellar Spectra As we saw in last week’s lab on light, stars, including the Sun, produce light by their heat and then that light travels through the star’s atmosphere which leaves absorption lines in the otherwise continuous spectrum. From these spectra we get two types of information. From the brightest color in the continuous spectrum, which is produced by the star’s heat, we can learn about the temperature of the star. From wavelengths of the dark lines in the spectrum we can learn about what types of materials exist in the star’s atmosphere. In this lab we will look at spectra of the 7 classes of main sequence stars and sort them by their temperatures and line patterns. ATTACHMENT PREVIEW Download attachment Spectrum_of_Stars_Back_ground_info_2.png VEGA Wavelength (nanometers) Above is a sample spectrum of the star Vega. At the top is the spectrum the way it might appear in your spectrometer. Below is a different representation of the spectrum showing the light intensity of the spectrum as a function of wavelength. Where the line rises up high you know that the star produces a lot of light at that color. Where the line drops less light is being produced. The star Vega produces a lot of light in the violet around 400 nm and is relatively faint at both shorter violet wavelengths and the longer red wavelengths. The black absorption lines in the spectrum show up as dips in the intensity graph, wavelength values where the spectrum goes dark. The line in the red box is the Balmer Hydrogen line. Lines can be produced by many different elements and show up at many different places in the spectrum but the one at 656 nm marked by the red box is produced by hydrogen. The peak wavelength of Amax is the brightest wavelength. The wavelength at which the intensity of light is highest. In the case of Vega, Amax, marked by blue lines, is about 405 nm. In this lab we will start by looking at examples of spectra from 7 different classes of main sequence stars. In each case you will be asked to find Amax the brightest color, to identify the wavelengths of the main lines in the spectrum, and to determine the relative strength of th Balmer hydrogen line. I will do the first one for you as an example. The color spectra come from an image published by NOAO/AURA/NSF and the line spectra are from the Astrophysical Journal Supplement Series, 56; 257-281, 1984 October. Both are provided by the NASA Astrophysics Data System. ATTACHMENT PREVIEW Download attachment Spectrum_of_Stars_Back_ground_info_3.png Star name

Spectrum of Stars q2Background src=”/qa/attachment/8320106/” alt=”Spectrum_of_Stars_Back_ground_info_1.png” />QUESTION Attachment 1 Attachment

Question Spectrum of Stars q2Background src=”/qa/attachment/8320106/” alt=”Spectrum_of_Stars_Back_ground_info_1.png” />QUESTION Attachment 1 Attachment 2 Attachment 3 Attachment 4 ATTACHMENT PREVIEW Download attachment Spectrum_of_Stars_Back_ground_info_1.png Stellar Spectra As we saw in last week’s lab on light, stars, including the Sun, produce light by their heat and then that light travels through the star’s atmosphere which leaves absorption lines in the otherwise continuous spectrum. From these spectra we get two types of information. From the brightest color in the continuous spectrum, which is produced by the star’s heat, we can learn about the temperature of the star. From wavelengths of the dark lines in the spectrum we can learn about what types of materials exist in the star’s atmosphere. In this lab we will look at spectra of the 7 classes of main sequence stars and sort them by their temperatures and line patterns. ATTACHMENT PREVIEW Download attachment Spectrum_of_Stars_Back_ground_info_2.png VEGA Wavelength (nanometers) Above is a sample spectrum of the star Vega. At the top is the spectrum the way it might appear in your spectrometer. Below is a different representation of the spectrum showing the light intensity of the spectrum as a function of wavelength. Where the line rises up high you know that the star produces a lot of light at that color. Where the line drops less light is being produced. The star Vega produces a lot of light in the violet around 400 nm and is relatively faint at both shorter violet wavelengths and the longer red wavelengths. The black absorption lines in the spectrum show up as dips in the intensity graph, wavelength values where the spectrum goes dark. The line in the red box is the Balmer Hydrogen line. Lines can be produced by many different elements and show up at many different places in the spectrum but the one at 656 nm marked by the red box is produced by hydrogen. The peak wavelength of Amax is the brightest wavelength. The wavelength at which the intensity of light is highest. In the case of Vega, Amax, marked by blue lines, is about 405 nm. In this lab we will start by looking at examples of spectra from 7 different classes of main sequence stars. In each case you will be asked to find Amax the brightest color, to identify the wavelengths of the main lines in the spectrum, and to determine the relative strength of th Balmer hydrogen line. I will do the first one for you as an example. The color spectra come from an image published by NOAO/AURA/NSF and the line spectra are from the Astrophysical Journal Supplement Series, 56; 257-281, 1984 October. Both are provided by the NASA Astrophysics Data System. ATTACHMENT PREVIEW Download attachment Spectrum_of_Stars_Back_ground_info_3.png Star name

Spectrum of Stars q3BACKGROUND alt=”Spectrum_of_Stars_Back_ground_info_1.png” />QUESTION: Attachment 1 Attachment 2

Question Spectrum of Stars q3BACKGROUND alt=”Spectrum_of_Stars_Back_ground_info_1.png” />QUESTION: Attachment 1 Attachment 2 Attachment 3 Attachment 4 ATTACHMENT PREVIEW Download attachment Spectrum_of_Stars_Back_ground_info_1.png Stellar Spectra As we saw in last week’s lab on light, stars, including the Sun, produce light by their heat and then that light travels through the star’s atmosphere which leaves absorption lines in the otherwise continuous spectrum. From these spectra we get two types of information. From the brightest color in the continuous spectrum, which is produced by the star’s heat, we can learn about the temperature of the star. From wavelengths of the dark lines in the spectrum we can learn about what types of materials exist in the star’s atmosphere. In this lab we will look at spectra of the 7 classes of main sequence stars and sort them by their temperatures and line patterns. ATTACHMENT PREVIEW Download attachment Spectrum_of_Stars_Back_ground_info_2.png VEGA Wavelength (nanometers) Above is a sample spectrum of the star Vega. At the top is the spectrum the way it might appear in your spectrometer. Below is a different representation of the spectrum showing the light intensity of the spectrum as a function of wavelength. Where the line rises up high you know that the star produces a lot of light at that color. Where the line drops less light is being produced. The star Vega produces a lot of light in the violet around 400 nm and is relatively faint at both shorter violet wavelengths and the longer red wavelengths. The black absorption lines in the spectrum show up as dips in the intensity graph, wavelength values where the spectrum goes dark. The line in the red box is the Balmer Hydrogen line. Lines can be produced by many different elements and show up at many different places in the spectrum but the one at 656 nm marked by the red box is produced by hydrogen. The peak wavelength of Amax is the brightest wavelength. The wavelength at which the intensity of light is highest. In the case of Vega, Amax, marked by blue lines, is about 405 nm. In this lab we will start by looking at examples of spectra from 7 different classes of main sequence stars. In each case you will be asked to find Amax the brightest color, to identify the wavelengths of the main lines in the spectrum, and to determine the relative strength of th Balmer hydrogen line. I will do the first one for you as an example. The color spectra come from an image published by NOAO/AURA/NSF and the line spectra are from the Astrophysical Journal Supplement Series, 56; 257-281, 1984 October. Both are provided by the NASA Astrophysics Data System. ATTACHMENT PREVIEW Download attachment Spectrum_of_Stars_Back_ground_info_3.png Star name

Spectrum of Stars q4BACKGROUND alt=”Spectrum_of_Stars_Back_ground_info_1.png” />QUESTION Attachment 1 Attachment 2

Question Spectrum of Stars q4BACKGROUND alt=”Spectrum_of_Stars_Back_ground_info_1.png” />QUESTION Attachment 1 Attachment 2 Attachment 3 Attachment 4 ATTACHMENT PREVIEW Download attachment Spectrum_of_Stars_Back_ground_info_1.png Stellar Spectra As we saw in last week’s lab on light, stars, including the Sun, produce light by their heat and then that light travels through the star’s atmosphere which leaves absorption lines in the otherwise continuous spectrum. From these spectra we get two types of information. From the brightest color in the continuous spectrum, which is produced by the star’s heat, we can learn about the temperature of the star. From wavelengths of the dark lines in the spectrum we can learn about what types of materials exist in the star’s atmosphere. In this lab we will look at spectra of the 7 classes of main sequence stars and sort them by their temperatures and line patterns. ATTACHMENT PREVIEW Download attachment Spectrum_of_Stars_Back_ground_info_2.png VEGA Wavelength (nanometers) Above is a sample spectrum of the star Vega. At the top is the spectrum the way it might appear in your spectrometer. Below is a different representation of the spectrum showing the light intensity of the spectrum as a function of wavelength. Where the line rises up high you know that the star produces a lot of light at that color. Where the line drops less light is being produced. The star Vega produces a lot of light in the violet around 400 nm and is relatively faint at both shorter violet wavelengths and the longer red wavelengths. The black absorption lines in the spectrum show up as dips in the intensity graph, wavelength values where the spectrum goes dark. The line in the red box is the Balmer Hydrogen line. Lines can be produced by many different elements and show up at many different places in the spectrum but the one at 656 nm marked by the red box is produced by hydrogen. The peak wavelength of Amax is the brightest wavelength. The wavelength at which the intensity of light is highest. In the case of Vega, Amax, marked by blue lines, is about 405 nm. In this lab we will start by looking at examples of spectra from 7 different classes of main sequence stars. In each case you will be asked to find Amax the brightest color, to identify the wavelengths of the main lines in the spectrum, and to determine the relative strength of th Balmer hydrogen line. I will do the first one for you as an example. The color spectra come from an image published by NOAO/AURA/NSF and the line spectra are from the Astrophysical Journal Supplement Series, 56; 257-281, 1984 October. Both are provided by the NASA Astrophysics Data System. ATTACHMENT PREVIEW Download attachment Spectrum_of_Stars_Back_ground_info_3.png Star name

Spectrum of Stars q5BACKGROUND src=”/qa/attachment/8320121/” alt=”Spectrum_of_Stars_Back_ground_info_1.png” />QUESTION Attachment 1 Attachment

Question Spectrum of Stars q5BACKGROUND src=”/qa/attachment/8320121/” alt=”Spectrum_of_Stars_Back_ground_info_1.png” />QUESTION Attachment 1 Attachment 2 Attachment 3 Attachment 4 ATTACHMENT PREVIEW Download attachment Spectrum_of_Stars_Back_ground_info_1.png Stellar Spectra As we saw in last week’s lab on light, stars, including the Sun, produce light by their heat and then that light travels through the star’s atmosphere which leaves absorption lines in the otherwise continuous spectrum. From these spectra we get two types of information. From the brightest color in the continuous spectrum, which is produced by the star’s heat, we can learn about the temperature of the star. From wavelengths of the dark lines in the spectrum we can learn about what types of materials exist in the star’s atmosphere. In this lab we will look at spectra of the 7 classes of main sequence stars and sort them by their temperatures and line patterns. ATTACHMENT PREVIEW Download attachment Spectrum_of_Stars_Back_ground_info_2.png VEGA Wavelength (nanometers) Above is a sample spectrum of the star Vega. At the top is the spectrum the way it might appear in your spectrometer. Below is a different representation of the spectrum showing the light intensity of the spectrum as a function of wavelength. Where the line rises up high you know that the star produces a lot of light at that color. Where the line drops less light is being produced. The star Vega produces a lot of light in the violet around 400 nm and is relatively faint at both shorter violet wavelengths and the longer red wavelengths. The black absorption lines in the spectrum show up as dips in the intensity graph, wavelength values where the spectrum goes dark. The line in the red box is the Balmer Hydrogen line. Lines can be produced by many different elements and show up at many different places in the spectrum but the one at 656 nm marked by the red box is produced by hydrogen. The peak wavelength of Amax is the brightest wavelength. The wavelength at which the intensity of light is highest. In the case of Vega, Amax, marked by blue lines, is about 405 nm. In this lab we will start by looking at examples of spectra from 7 different classes of main sequence stars. In each case you will be asked to find Amax the brightest color, to identify the wavelengths of the main lines in the spectrum, and to determine the relative strength of th Balmer hydrogen line. I will do the first one for you as an example. The color spectra come from an image published by NOAO/AURA/NSF and the line spectra are from the Astrophysical Journal Supplement Series, 56; 257-281, 1984 October. Both are provided by the NASA Astrophysics Data System. ATTACHMENT PREVIEW Download attachment Spectrum_of_Stars_Back_ground_info_3.png Star name

how does the post-main-sequence evolution of a low-mass star differ

Question how does the post-main-sequence evolution of a low-mass star differ from that of a high-mass star? What stellar remnants are associated with each? 

Which of the following provide direct observational evidence in support

Question Which of the following provide direct observational evidence in support of the Big Bang Theory? Choose all that apply.The abundance of elements in the distant/early universethe existence of black holesThe existence of the main sequenceThe Cosmic Microwave BackgroundThe expansion of the Universethe existence of spiral galaxiesstellar evolutionstellar parallax

In this graph the brightest wavelength, λmax, is about 3800

Question In this graph the brightest wavelength, λmax, is about 3800 angstroms (Å) (10 Å equals 1 nm so 3800 Å is 380 nm) and it is brightest in the blue, blue/green colors. The spectrum has many dark lines in the blue part of the spectrum, particularly at 4850, 4350, 4100, 3950, 3900, and 3850 Å. There are a few weaker lines, two in the yellow that can be seen the color spectrum. The Balmer hydrogen line (red box/arrow) is noticeable but not especially strong. ATTACHMENT PREVIEW Download attachment Grumpy.png

Q1 analyze the spectra below. When finding the peak wavelength

Question Q1 analyze the spectra below. When finding the peak wavelength use the top spectrum. Identify the wavelength for λmax and other prominent lines. Identify the brightest color and discuss the overall line pattern. Discuss the relative strength of the Balmer hydrogen line. When considering the Balmer line compare it with the Balmer lines from some of the other spectral types rather than comparing with other lines from the same star. ATTACHMENT PREVIEW Download attachment sleepy.png

The post What is a Balmer transition in a hydrogen molecule? What appeared first on Smashing Essays.

 
Looking for a Similar Assignment? Order now and Get 10% Discount! Use Coupon Code "Newclient"