Answer:
11625 miles
Explanation:
A second of light is the distance that light travels in a second. It has a value of 299792458 kilometers or if we do the unit conversion, 186,000 miles. A mile is 1.609 kilometers
Let's make a rule of three:
1 light s travels a distance of 186000 miles
0.062500 light s would travel a distance of (0.062500 . 186000) = 11625 miles
A crushed garlic will have a lot of flavor when placed in food due to the surface area that is in contact with the food. When we have a large piece of garlic, only the external part touches the food and its full capacity is not used. When we reduce the size of the year by crushing the internal parts that were not in contact with the food, now they will be, in addition, liquids are also released due to the pressure exerted on the garlic and these liquids mix more easily with the food and they give it more flavor. For better understanding we can see the following figure:
Simply to understand it, in the figure, there is a clove of whole garlic represented by the rectangle that will have a height of 3 and a width of 1, the units do not matter in this case. The area that is in contact will be equal to 8, but if we divide the garlic into three equal parts, it will have a contact area greater than 12. Therefore, the more we divide the garlic, the more area it will be in contact with the food and will give it more flavor.
The number of carbon atoms present in any compound is equal to seven.
<h3>How do we calculate the number of carbon atoms?</h3>
Number of carbon atoms present in any compound will be calculated by using the following equation:
No. of Carbon atoms = Relative intensity of M+1 peak / Natural abundance of C13
Intensity of molecular peak = 34.76%
Intensity of M+1 peak = 2.632%
Relative intensity of M+1 peak = (100/34.76)×2.632 = 7.57%
Given that natural abundance of M+1 = 1.07%
On putting values on above equation, we get
No. of C atoms = 7.57 / 1.07 = 7.07 = 7 (approx)
Hence number of carbon atoms is 7.
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Answer:In general, yes. Usually, you talk about the reflectivity/emissivity of a surface rather than an object. Typically, you’d find a coefficient of emissivity (since emission and absorption are normally equivalent processes in reverse) for the surface, ideally as a function of wavelength and incident angle. Then you apply that coefficient to all light striking the object.
Assuming an opaque object, reflectivity (call it R) has a simple relationship to emissivity (call it E): R=1-E. You can measure reflectivity with a calibrated light source and light sensor, for example. It’s a little trickier, but you can also measure emissivity through techniques like calorimetry, where you measure how much something heats up to figure out how much energy was deposited; again, a calibrated light source can be used to direct a certain amount of power onto a test object, and the heating tells you how much power is retained. You can also get emissivity by heating an object and observing how much power it emits by blackbody radiation.
To be really thorough, you might also want to measure transmissivity, in case the object isn’t opaque. If we call transmissivity “T,” we really have to write R+E+T=1 (which just says that all the incident light has to either reflect, absorb, or pass through).
If the object is something celestial, of course, it’s harder to use these methods, but not impossible. For example, we can measure how much light the full moon reflects, and knowing how much light hits it from the sun, we can find the reflectivity; in principle, we could use our knowledge of how much the surface of the moon is heated by the sun to find the emissivity, as well. For that kind of calculation, it’s important to know how large and how distant an object is, to figure out how much of its reflected light makes it back to you.
Explanation:
