0.00032cm*4.02=1.2864 × 10^-3 in scientific notation.
Although the sample is not shown in this question, we can conclude that it would be reasonably easy for David to provide evidence of the color, consistency, temperature, and texture of the soil.
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<h3>What are these properties an example of?</h3>
These are all examples of the physical properties of a sample. Since we cannot see the sample that David is using, it would be safest to assume that he would have no trouble providing evidence as to the physical properties of the soil, the:
- Color
- Consistency
- Temperature
- Texture
are all examples of this.
Therefore, we can confirm that David can provide evidence of the color, consistency, temperature, and texture of the soil.
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Answer:
0.125 m
Explanation:
Pressure in fluids is given as the product of density, height and acceleration due to gravity and expressed as
P=hdg
Where h is the height, d is density, g is acceleration due to gravity and P is pressure.
Making h the subject of formula then
h=P/dg
Given specific gravity of a substance, its density is equal to specific gravity multiplied by density of water. Taking density of pure water as 1000 kg/m³ then the density of reference fluid will be 1.05*1000=1050 kg/m³
Substituting pressure with 1.29*10³ pa as given then taking g as 9.81 m/s² then
H=1.29*10³÷(9.81*1050)=0.1252366389981068880151448958788408329692m
Rounded off, the height is approximately 0.125 m
Answer: 
Explanation:
This problem can be solved using the Third Kepler’s Law of Planetary motion:
<em>“The square of the orbital period of a planet is proportional to the cube of the semi-major axis (size) of its orbit”. </em>
<em />
This law states a relation between the orbital period
of a body (the exoplanet in this case) orbiting a greater body in space (the star in this case) with the size
of its orbit:
(1)
Where:
is the period of the orbit of the exoplanet (considering
)
is the Gravitational Constant and its value is
is the mass of the star
is orbital radius of the orbit the exoplanet describes around its star.
Now, if we want to find the radius, we have to rewrite (1) as:
(2)
(3)
Finally:
This is the radius of the exoplanet's orbit