The chemical energy in Jay's body, to kinetic energy in the car
Hello! You can call me Emac or Eric.
I understand your problem, that question is pretty hard. But I found some information that I think you should read. This can get your problem done quickly.
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Please reply if this doesn’t help, I will try my best to gather more information or a answer.
Here is some good information that could help you out a lot!
Let’s begin by exploring some techniques astronomers use to study how galaxies are born and change over cosmic time. Suppose you wanted to understand how adult humans got to be the way they are. If you were very dedicated and patient, you could actually observe a sample of babies from birth, following them through childhood, adolescence, and into adulthood, and making basic measurements such as their heights, weights, and the proportional sizes of different parts of their bodies to understand how they change over time.
Unfortunately, we have no such possibility for understanding how galaxies grow and change over time: in a human lifetime—or even over the entire history of human civilization—individual galaxies change hardly at all. We need other tools than just patiently observing single galaxies in order to study and understand those long, slow changes.
We do, however, have one remarkable asset in studying galactic evolution. As we have seen, the universe itself is a kind of time machine that permits us to observe remote galaxies as they were long ago. For the closest galaxies, like the Andromeda galaxy, the time the light takes to reach us is on the order of a few hundred thousand to a few million years. Typically not much changes over times that short—individual stars in the galaxy may be born or die, but the overall structure and appearance of the galaxy will remain the same. But we have observed galaxies so far away that we are seeing them as they were when the light left them more than 10 billion years ago.
That is some information, I do have more if you need some! Thanks!
Have a great rest of your day/night! :)
Emacathy,
Brainly Team.
Answer:
Chemical composition, Temperature, Radial velocity, Size or diameter of the star, Rotation.
Explanation:
Elemental abundances are determined by analyzing the relative strengths of the absorption lines in the spectrum of a star.
The Spectral class to which the star belongs gives the information related to the temperature of the star. It is the spectral lines that determine the spectral class O B A F G K M are the spectral classes.
By measuring the wavelengths of the lines in the star's spectrum gives the radial velocity. Doppler shift is the method used to find the radial velocity.
A star can be classified as a giant or a dwarf . A giant star will have narrow width spectral lines whereas a dwarf star has wider spectral lines.
Broadening of the spectral lines will determine the star's rotation.
Answer
given,
diameter,d₁ = 7.5 cm
d₂ = 4.5 cm
P₁ = 32 kPa
P₂ = 25 kPa
Assuming, we have calculation of flow in the pipe
using continuity equation
A₁ v₁ = A₂ v₂
π r₁² v₁ = π r₂² v₂
Applying Bernoulli's equation
v₂ = 4.01 m/s
fluid flow rate
Q = A₂ V₂
Q = π (0.0225)² x 4.01
Q = 6.38 x 10⁻³ m³/s
flow in the pipe is equal to 6.38 x 10⁻³ m³/s
Answer:
1.6 m/s²
Explanation:
Weight equals mass times acceleration due to gravity.
F = mg
14.4 N = (9 kg) g
g = 1.6 m/s²
