The Moon has no sustained atmosphere. What advantages would you have if you built an
observatory on the lunar surface? (Select all that apply.)
Without atmospheric turbulence, there would be no image blur due to seeing.
There is no atmosphere to absorb or scatter radiation, so all wavelengths of light could be
observed with lunar-based telescopes, from radio waves to gamma rays.
The Moon is closer to many stars than the Earth, and lunar-based telescopes would produce
images with more detail based on this closer proximity.
On Earth, large mirrors in telescopes can sag under their own weight. Without an atmosphere to
apply pressure, mirrors on the Moon would not sag.
We could observe continuously because there would never be any clouds.
We could observe during the day. Without an atmosphere, sunlight is not scattered and the sky
remains dark.
Distortion of mirrors due to temperature shifts would no longer be an issue, without an
atmosphere to retain the heat from sunlight..
This workshop introduces 10-13 years old children to space weather, solar-flare forecasting and the SunSpotter citizen science project.
Hanna Sathiapal, FLARECAST outreach 2015-2017
This is a workshop introducing participants to solar observation and forecasting solar flares preparing them to contribute to the Sunspotter citizen science project. Developed in the context of the FLARECAST public engagement programme, it can be used by anyone interested in communicating solar science.
This workshop introduces 10-13 years old children to space weather, solar-flare forecasting and the SunSpotter citizen science project.
Hanna Sathiapal, FLARECAST outreach 2015-2017
This is a workshop introducing participants to solar observation and forecasting solar flares preparing them to contribute to the Sunspotter citizen science project. Developed in the context of the FLARECAST public engagement programme, it can be used by anyone interested in communicating solar science.
James Webb Telescope: Pioneering the Frontier of Space Exploration524RohitBhupalam
Embark on an awe-inspiring journey that traverses both space and time, all thanks to the incredible James Webb Telescope! 🌌✨
Prepare for wonderment as we delve into the inner workings of this remarkable telescope and the ingenious solutions that brilliant scientists found to overcome formidable challenges. Our presentation is a gallery of mesmerizing images, each captured by the telescope—a visual feast showcasing galaxies, stars, and celestial marvels, all of which could easily be mistaken as art.
However, what truly sets the James Webb Telescope apart is its ability to grant us a glimpse into the past. Imagine a time machine that allows us to observe the universe as it existed billions of years ago, unraveling the very beginning of cosmic evolution. 🕰️⏳ As we peel back the layers, you'll discover how this remarkable feat is achieved, forever altering our perception of the cosmos and the events that shaped it.
Join us on this extraordinary expedition as we navigate the cosmos, guided by the James Webb Telescope's unerring gaze. 🚀🔭✨ Prepare to be not only amazed but also stirred with an curiosity that will forever change the way you perceive the universe around us.
I can analyze the differences between comets, asteroids, meteors and moons. I will research orbits and discuss differences of what we see from the Earth’s surface (phases). I will analyze the effect the moon’s orbit has on our planet. I will predict what would happen if Earth had a 2nd moon or the distance to the moon was increased or decreased.
Astronomy 161 – Spectroscopy Lab Introduction The li.docxrock73
Astronomy 161 – Spectroscopy Lab
Introduction:
The light of celestial objects contains much information hidden in its detailed color
structure. In this lab we will separate the light from some sources into constituent colors and use
spectroscopy to find out the chemical constitution of known and unknown gases. The same
procedure is used for starlight, telling us what its source is composed of. The baseline is a
laboratory experiment with known materials, and later we can compare the unknown to what we
already know.
Hot, glowing bodies like a light
bulb, or the Sun, glow in all the colors of
the spectrum. All these colors together
appear as white light. When such white
light hits a prism, or a raindrop, or a
diffraction grating, colors get separated
according to their wavelength. Red, with
its wavelength of 600 nm to 700 nm, is
deflected least and ends up on one edge of
the spectrum – or the rainbow when sunlight hits a raindrop after a storm. Blue, wavelength
around 400 nm, is the other end of the visible spectrum. An infinite number of elementary colors
are located between these two edges, each corresponding to its own wavelength. An
incandescent light bulb radiates a continuous spectrum. All colors are present in this “thermal
glow”, and it is impossible to tell what the chemical composition of the source is.
However, other physical processes produce different spectra. A fluorescent light tube
works, crudely speaking, on the principle of lightening. Electrons rush from the negative pole to
the positive pole inside, and hit gas atoms in the tube, making them emit light. This sort of light
contains only a few colors, and is called “emission spectrum”. When we separate the colors of
such light, only a few bright “emission” lines appear, each in its own color (and wavelength).
Each sort of an atom will emit light at its own particular set of wavelengths. When we analyze
the emission spectrum of an unknown source, we can compare the colors of its spectral lines to
known spectral lines we see in a laboratory, and tell which substance matches.
The color of spectral lines is directly
related to the structure of the atoms. Electrons
can jump from one orbit around the atomic
nucleus to another, giving off the difference in
energy levels in the form of light. The
wavelength (color) of light is related to the
amount of energy freed up between the old and
the new orbit. In this laboratory we will measure
the wavelengths of spectral lines from a few
gases, which are easy to put inside a discharge
tube. Other chemical elements would have
different spectra.
In the spectroscope that we use in this
laboratory, a diffraction grating (many parallel
black lines drawn very tightly on a little piece of
film) breaks up the light entering through the input slit into colored lines. Each color corresponds
to a wavelength, measured in nanometers (1 nm = 10-9 m).
Instructions:
In
this
investigation
...
The model (graph) below represents a small country trade of coffee- Be.pdfaarastore
The model (graph) below represents a small country trade of coffee. Before trade, what area(s)
represent consumer's surplus? a. G b. C + F C. A + B + D d. A only.
The mode of inheritance you are to test on the observed data is autoso.pdfaarastore
The mode of inheritance you are to test on the observed data is autosomat dominant.
PARENTAL CROSS Parental crosst Nother with disease phenotype, Father with wid-type
phenotype. F. DATA F2 DATA Phenotype Disease Mitd-Type 45 For your assignment, you are
provided with F 1 data as well as F 2 data. Given that the F 1 data come from a cross of an
affected parent with an unaffected parent who is homozygous for the wild-type allele, and given
that you have studied many crosses this semester, state what you think is the true mode of
inheritance for your disease, and provide an answer using the observed data. Note that what you
think may be different from the mode of inheritance provided in the assignment..
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Embark on an awe-inspiring journey that traverses both space and time, all thanks to the incredible James Webb Telescope! 🌌✨
Prepare for wonderment as we delve into the inner workings of this remarkable telescope and the ingenious solutions that brilliant scientists found to overcome formidable challenges. Our presentation is a gallery of mesmerizing images, each captured by the telescope—a visual feast showcasing galaxies, stars, and celestial marvels, all of which could easily be mistaken as art.
However, what truly sets the James Webb Telescope apart is its ability to grant us a glimpse into the past. Imagine a time machine that allows us to observe the universe as it existed billions of years ago, unraveling the very beginning of cosmic evolution. 🕰️⏳ As we peel back the layers, you'll discover how this remarkable feat is achieved, forever altering our perception of the cosmos and the events that shaped it.
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I can analyze the differences between comets, asteroids, meteors and moons. I will research orbits and discuss differences of what we see from the Earth’s surface (phases). I will analyze the effect the moon’s orbit has on our planet. I will predict what would happen if Earth had a 2nd moon or the distance to the moon was increased or decreased.
Astronomy 161 – Spectroscopy Lab Introduction The li.docxrock73
Astronomy 161 – Spectroscopy Lab
Introduction:
The light of celestial objects contains much information hidden in its detailed color
structure. In this lab we will separate the light from some sources into constituent colors and use
spectroscopy to find out the chemical constitution of known and unknown gases. The same
procedure is used for starlight, telling us what its source is composed of. The baseline is a
laboratory experiment with known materials, and later we can compare the unknown to what we
already know.
Hot, glowing bodies like a light
bulb, or the Sun, glow in all the colors of
the spectrum. All these colors together
appear as white light. When such white
light hits a prism, or a raindrop, or a
diffraction grating, colors get separated
according to their wavelength. Red, with
its wavelength of 600 nm to 700 nm, is
deflected least and ends up on one edge of
the spectrum – or the rainbow when sunlight hits a raindrop after a storm. Blue, wavelength
around 400 nm, is the other end of the visible spectrum. An infinite number of elementary colors
are located between these two edges, each corresponding to its own wavelength. An
incandescent light bulb radiates a continuous spectrum. All colors are present in this “thermal
glow”, and it is impossible to tell what the chemical composition of the source is.
However, other physical processes produce different spectra. A fluorescent light tube
works, crudely speaking, on the principle of lightening. Electrons rush from the negative pole to
the positive pole inside, and hit gas atoms in the tube, making them emit light. This sort of light
contains only a few colors, and is called “emission spectrum”. When we separate the colors of
such light, only a few bright “emission” lines appear, each in its own color (and wavelength).
Each sort of an atom will emit light at its own particular set of wavelengths. When we analyze
the emission spectrum of an unknown source, we can compare the colors of its spectral lines to
known spectral lines we see in a laboratory, and tell which substance matches.
The color of spectral lines is directly
related to the structure of the atoms. Electrons
can jump from one orbit around the atomic
nucleus to another, giving off the difference in
energy levels in the form of light. The
wavelength (color) of light is related to the
amount of energy freed up between the old and
the new orbit. In this laboratory we will measure
the wavelengths of spectral lines from a few
gases, which are easy to put inside a discharge
tube. Other chemical elements would have
different spectra.
In the spectroscope that we use in this
laboratory, a diffraction grating (many parallel
black lines drawn very tightly on a little piece of
film) breaks up the light entering through the input slit into colored lines. Each color corresponds
to a wavelength, measured in nanometers (1 nm = 10-9 m).
Instructions:
In
this
investigation
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The Moon has no sustained atmosphere- What advantages would you have i.pdf
1. The Moon has no sustained atmosphere. What advantages would you have if you built an
observatory on the lunar surface? (Select all that apply.)
Without atmospheric turbulence, there would be no image blur due to seeing.
There is no atmosphere to absorb or scatter radiation, so all wavelengths of light could be
observed with lunar-based telescopes, from radio waves to gamma rays.
The Moon is closer to many stars than the Earth, and lunar-based telescopes would produce
images with more detail based on this closer proximity.
On Earth, large mirrors in telescopes can sag under their own weight. Without an atmosphere to
apply pressure, mirrors on the Moon would not sag.
We could observe continuously because there would never be any clouds.
We could observe during the day. Without an atmosphere, sunlight is not scattered and the sky
remains dark.
Distortion of mirrors due to temperature shifts would no longer be an issue, without an
atmosphere to retain the heat from sunlight.
