Answer:
The distance of stars and the earth can be averagely measured by using the knowledge of geometry to estimate the stellar parallax angle(p).
From the equation below, the stars distances can be calculated.
D = 1/p
Distance = 1/(parallax angle)
Stellar parallax can be used to determine the distance of stars from an observer, on the surface of the earth due to the motion of the observer. It is the relative or apparent angular displacement of the star, due to the displacement of the observer.
Explanation:
Parallax is the observed apparent change in the position of an object resulting from a change in the position of the observer. Specifically, in the case of astronomy it refers to the apparent displacement of a nearby star as seen from an observer on Earth.
The parallax of an object can be used to approximate the distance to an object using the formula:
D = 1/p
Where p is the parallax angle observed using geometry and D is the actual distance measured in parsecs. A parsec is defined as the distance at which an object has a parallax of 1 arcsecond. This distance is approximately 3.26 light years
Answer:
Weather is the conditions (temperature, wind etc.) at a given time, like on that day. Climate, which is what his data would show, is the conditions over an extended period of time like the 3 months he collected data
The law of universal gravitation says that one object attracts every other object using a proportional force to the mass of the object.
Answer:
1.137278672 m/s
+5.9 cm or -5.9 cm
Explanation:
A = Amplitude = 6.25 cm
m = Mass of object = 225 g
k = Spring constant = 74.5 N/m
Maximum speed is given by

The maximum speed of the object is 1.137278672 m/s
Velocity is at any instant is given by

The locations are +5.9 cm or -5.9 cm
I attached the full question.
We need to calculate the enthalpy change first:

Keep in mind this is the energy per mole, we need energy per atom:

We can see that this reaction needs the energy to get started (enthalpy change is positive).
The energy of a photon is given with this formula:

We need this photon to have the same energy (or higher) as our enthalpy change:

This wavelenght is clasified as near infrared.