As the temperature rises, the average speed at which the molecules are moving the relationship between time and the average distance the particles have. And that amount in turn is inversely proportional to the square of distance from the Sun. So ultimately the object's temperature is inversely proportional to the. All bodies with a temperature greater than absolute zero radiate energy. Absolute and Boltzmann theoretically developed a relationship between the temperature emitting body's temperature, its size and its distance to the receiving body.
You will use the vScope to study a two basic properties of diffusion.
Temperature relationship to distance and flow rate of warmed i.v. fluids.
These are the relationship between time and the average distance the particles have traveled. To answer these question you need reliable data. These numbers will be part of your lab report! Perform at least three independent experiments using the vScope. Each experiment should be at least 30 seconds long. The simplest approach is to let the experiment run for about 33 second; stop it and then determine distance traveled at various time points e. Make a table of your data.
For each set of measurements, calculate the mean distance travelled and standard deviation for each time point. Hand in your graph with your report. If the relationship between time and distance is linear, then when the time is doubled, the average distance traveled will be doubled. If your data does not fall on a straight line there are two possibilities; it is not describable by a mathematical relationship or more likely the mathematical relationship that describes it is more complex than a simple linear relationship.
Perform at least 3 trials for each temperature, some may have to be longer than 30 seconds. Planets with no atmosphere For planets with no atmosphere all the Sun's radiation will strike the surface. Some of this will be reflected away from the planet but the rest will be absorbed.
How to calculate the expected surface temperature of a planet - Astronomy Stack Exchange
The temperature of the surface will be raised until there is equilibrium between the energy radiated by the warm surface of the planet and the received solar radiation. The Moon is similar in many ways to Mercury. Planets with atmospheres The Earth is, of course, a planet with an atmosphere and we can use it as an example. Our atmosphere is largely transparent to the incoming solar radiation although there are constituents in the atmosphere which prevent some kinds of radiation from reaching the surface, such as ozone which stops the ultraviolet.
A fair proportion of the Earth is covered by clouds which reflect a lot of the Sun's radiation and it has been postulated that drastic change in the amount of cloud could precipitate an ice-age thus dramatically affecting the surface temperature.
Carbon dioxide is the main constituent which does this and there are fears that increases in the amount of this gas in the atmosphere will cause global warming of the Earth and change its climatic patterns. The other main effect of the atmosphere, particularly when it is cloudy, is to trap the radiation from the Earth during the night, keeping the temperature fairly close to that in the day.
Venus is surrounded by clouds which prevent a lot of the Sun's radiation from reaching the surface and so we might have expected the surface to be cool. However, the atmosphere of Venus is largely composed of carbon dioxide which traps most of the radiation from the planet's surface. The planet Mars has an atmosphere but this has a surface pressure less than one hundredth of the Earth's.
With the following facts you can easily calculate the effective temperature of the Earth and, if you know the distance to the other planets, their effective temperatures as well. Lets walk through the steps together: Since we know the wavelength of the sun's maximum output we can use Wein's law to calculate the sun's temperature.
Relationship between PlanetTemperature and Distance from the Sun
Go ahead and do it. You should get a number near K, for convenience you can round this off to K.Differential Heating of Land and Water Surfaces - Class 5
If we know the sun's temperature we can calculate the intensity of the solar output Iflux per square meter, by using the Stephan Boltzman equation. Go ahead and calculate it.