Answer:
appearance, texture, color, odor, melting point, boiling point, density, solubility, polarity
Explanation:
Answer:
Minimum thickness; t = 9.75 x 10^(-8) m
Explanation:
We are given;
Wavelength of light;λ = 585 nm = 585 x 10^(-9)m
Refractive index of benzene;n = 1.5
Now, let's calculate the wavelength of the film;
Wavelength of film;λ_film = Wavelength of light/Refractive index of benzene
Thus; λ_film = 585 x 10^(-9)/1.5
λ_film = 39 x 10^(-8) m
Now, to find the thickness, we'll use the formula;
2t = ½m(λ_film)
Where;
t is the thickness of the film
m is an integer which we will take as 1
Thus;
2t = ½ x 1 x 39 x 10^(-8)
2t = 19.5 x 10^(-8)
Divide both sides by 2 to give;
t = 9.75 x 10^(-8) m
<h2>
Answer: The Big Bang theory</h2>
Explanation:
The Big Bang theory explains that billions of years ago, before the current universe was born, matter was concentrated in an infinitely small and highly dense point. Then, a large explosion caused this matter to expand in all directions, creating the universe we now know (including space and time).
In addition, this theory explains that our universe still continues its expansion process.
Answer:
Endothermic, because the reactants are lower in energy (C)
Explanation:
From the graph, you can see the energy of the products is higher than the energy of the reactants. If you recall that when the enthalpy change Eproducts is gretater than Ereactants, the reaction is said to be endothermic.
Answer:
temperature of about 2.72548 ± 0.00057 K.
Explanation:
The cosmic background radiation is an electromagnetic radiation that remains from an early stage of the universe during the big bang. It was accidentally discovered in 1965 by two American radio astronomers Arno Penzias and Robert Wilson. The radiation was given off before the formation of stars and planets, when the universe was young, denser, hotter, and filled with a uniform glow from a white-hot fog of hydrogen plasma, which cooled down as the universe expanded. From calculations, it was deduced that the radiation had a temperature of 2.72548±0.00057 K, which is close to the temperature of the universe during its formation.
