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Early physics classes often have you plug numbers in on the homework. But they have you do them by giving you big chunky numbers in SI units and so you can end up not knowing the scale of any of the numbers. If you have good professors later on, you will get to see the true joy of being able to roughly calculate the answer, and the way it lets you roughly understand the scale of things.

Some notes about physicsy numbers (I have memorized most of the numbers that I pull out of thin air, whereas anything I calculate is probably at best only roughly remembered):

The meter was originally defined as 1 millionth of the distance from the equator to the pole. So the circumference of the Earth is about 40 Mm (megameters, or thousands of km). You can then get that the radius is 6.5 Mm.

The Karman Line is a convention for the start of space, 100 km above sea level. A picture from space will see the airglow at about that altitude. The Armstrong limit is the altitude at which water boils at human body temperature (though you'll still die at lower altitudes unprotected), and is about 20 km which incidentally is about where the troposphere ends and the stratosphere begins. Commercial flights fly at about 10-15 km up.

An astronomical unit (sun-earth distance) is about 500 light seconds, or .15 trillion meters. The moon is like 1 light second away. Now look at scale model of the solar system https://solar.heimerng.dev/ . The Earth is tilted relative to the solar system by about 23 degrees, useful for astronomical calculations like predicting where stuff will be in the sky.

The gravitational constant G is very small. It's also hard to measure. Much easier to measure is G M where M is the mass of the Earth. This is because GM/R^2 = g, where R is the radius of the Earth and g is the gravitational acceleration on Earth (about 9.8 ≈ 10 m/s. It varies by location by up to almost 1%). So GM = 420 Trillion (m^3/s^2). To find M, use the fact (which Newton guesstimated surprisingly accurately!) that the average density of the Earth is about 5 times that of water (water has a density of 1 g/cm^3 = 1 g/mL = 1 kg/L = 1 ton/m^3, which originally was how the kilogram was defined) (additionally, air's density is about a thousandth of water). From this you can find the volume (1 trillion trillion m^3) and mass (6 trillion trillion kg) of the Earth, and then the gravitational constant (about 70 per trillion in SI units).

Any physicist should know that the speed of light is very close to 3 * 10^8 (that is, 300 million) meters per second. This is about a foot per nanosecond. Funnily enough, this is how I remember that a foot is .3 meters. For the wavelength of visible light: green is 500 nm, +200 on the high end and -100 on the low end. Same is true for frequency, but this time in THz. You can check that 500 nm * 500 THz = 2.5 * 10^8 which is close to the speed of light. Visible light photons have an energy of about 2 (+1 on the high end, -.5 on the low end) eV. It takes like a dozen eVs to free electrons from metals.

Refractive indices are in a small range: water and glass are like 1.5, and at the high end diamond is like 2.5. Gases are very close to 1.

I can never remember the value of the (reduced) plank's constant ħ, the basic constant in quantum physics. It was amazing when a professor in a nuclear physics class gave me the following mneumonic: the product ħc is about 200 MeV fm (fm is femtometer, that is, 10^-15 meters). This is useful because I know how big c is, so whenever ħ pops up I can multiply and divide by c.

The binding energy, as any physicist knows, of a ground state electron in the hydrogen atom is 13.6 eV (that is, electron volts). You can just remember "a dozen". Thus, chemistry happens on the energy scale of 1-10 eVs. Likewise, our electron is .5 Angstroms away from the nucleus (an angstrom is .1 nanometers). So, chemistry happens on the scale of angstroms. X rays can probe things like crystal structure because they have a wavelength of around an angstrom (.1 nm, so frequencies of exahertz (10^18) and energies around 10 keV). Molecules tend to be that big. Proteins are more like dozens of angstroms, though and "weighs in" at 50k daltons (the mass of an atom in daltons/atomic mass units is about the number of nucleons it has, e.g. carbon-12 is 12 daltons) due to having like 5k atoms. There is an distinction in medicine/biology between "small molecules" (with <500 daltons) and "big molecules" like proteins.

Electrons bop about on the order of attoseconds (10^-18) (e.g. the time for a bond to form), while reactions happen on the order of hundreds of femtoseconds (10^-21, or 1k attoseconds). Femtosecond and even attosecond laser pulses can be made.

The molecules rotate and vibrate at energies on the order of meV, which is why infrared spectroscopy allows us to learn about that. Ultraviolet light at the far end can get high enough to ionize the electrons, starting at about 10 eV (100 nm or 1 PHz)

The electrostatic force/energy between two charged particles is given by coulomb's law. In SI units Coulomb's constant is 9 GJ m/Coulomb^2. For atomic physics, it's more useful to know that this is about 1 eV nm/e^2 (e is the magnitude of the charge of an electron). This tracks with the way that chemistry involves eVs and nms. Incidentally this is one way to remember how big an electron's charge, but instead I prefer using the Faraday constant: a mole (6 * 10^23) of electrons has about 100 kC of charge. Thus you can get that an electron has about 100/6 * 10^-19 = 1.6 * 10^-19 C.

A mole is the number of hydrogen atoms you need to have a gram of hydrogen, and thus converts between daltons and grams and is used a lot in chemistry. Numerically, it is about 6 * 10^23.

For the magnetic force: The vacuum permeability mu_0 is about 4 pi /10 micro Henries/m. The force between two infinitely long wires is the product of their currents times mu_0/(2 pi), that is, about .2 micro newtons per meter. "micro" is often denoted with the same greek letter, mu, which might help you remember.

Ferromagnetic core solenoids can't get above about 2 Tesla because of magnetic saturation. More than that and you are probably using a superconductor. You can levitate a frog with 15.

Nuclear physics happens on the scale of MeV. Binding energy differences per nucleon are a few of those, and this is why nuclear reactions are so powerful (e.g. fission for uranium-235 is 215 MeV). Gamma rays are often in the range of MeV As for size, nuclear physics happens on the femtometer (10^(-15) m) scale.

High energy physics smashes particles together and makes new ones. Electrons are .5 MeV in mass, while protons and neutrons are 1 GeV. The up and down quarks are a couple MeV, strange is like 100 MeV, and the rest are in the GeVs, which is why strange quarks show up more often.

In thermodynamics, the boltzmann constant comes up a lot. It converts between temperature (in kelvin. room temp is 20 C = 293 K) and energy. The "mole version" of it converts between temperature and the average energy of a mole of particles, and is called the ideal gas constant R. This is about 8 Joules/Kelvin/mol. Using this you can figure out that the boltzmann constant is on the scale of 10^(-23) in SI units. You can remember that at room temperature a monatomic ideal gas atom will have an average energy of 3/2 k_B T = 50 meV (actual number is 38), or alternatively that k_B T = 25 meV, and now you have a way to figure out how big an eV is. A mol of gas atoms will have 3/2 R T = 3.5 kJ of average energy, or in other words RT = 2.3 kJ at room temperature.

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