Dr. Pepper. The famous 23 flavor soda, has a lot of spinoff products, such as Diet Dr. Pepper. That’s not the topic here today. No we’re not talking about Diet Dr. Pepper barbecue sauce. But what we are talking about, is hot Dr. Pepper. That’s right, hot Dr. Pepper was originally introduced in the 1960’s as a winter beverage. Here’s some advertisements from the 1960’s showing about about Hot Dr. Pepper. However, it was short lived. But you still don’t believe me? You think this is a joke? Just go to the facts and questions article on the Dr. Pepper website. Anyway, I’m going to teach you how to make it. All you need is a Dr. Pepper; a can or bottle will be fine. And just proceed to open it, but DON’T blow it up like I did. Cuz’ you know, Bad Dr. Pepper right there. Anyway, you want to heat up a pan, or anything, and just pour a little Dr. Pepper in there, as much as you want. Alright, and as soon as we did that, we’re gonna take a lemon and a knife and make a small slice, and then put it into the glass that you’re gonna pour the hot Dr. pepper in. When the Dr. Pepper starts sizzling or steaming up… That’s it. Just take it off, and pour it in your glass. And if you’re using a glass glass glass made of glass like I am, put it very slowly. Like, wait five seconds between each… Each spill, so it doesn’t melt, cus you know, when glass melts… Glass… yeah. Also if you try this at home, and your lemon makes a popping bubble, comment or like, heh, cuz you know, thumbs up for that. Just some more footage of the popping lemon… Yeah, and basically, this is hot Dr. Pepper. It tastes just like Dr. Pepper, only it’s hot, kind of like tea. Brings out the cherry flavor. Little carbonation, and I’ll see you next time. Later!
We don’t know much about neutrinos, but what we do know points to renegade particles that, despite their prevalence, are hard to pin down. Here are, in a nutshell, nine neutrino nuggets that scientists have figured out so far.
Neutrinos are super abundant. The shining sun sends 65 billion neutrinos per second per square centimeter to Earth. Neutrinos are the second most abundant particle in the universe. If we were to take a snapshot, we’d see that every cubic centimeter has approximately 1,000 photons and 300 neutrinos
Neutrinos are almost massless. No one yet knows the mass of neutrinos, but it is at least a million times less massive than the lightest particle we know, the electron. We do know that each is so lightweight and so abundant that the total mass of all neutrinos in the universe is estimated to be equal to the total mass of all of the visible stars. (To learn more about the neutrino masses click here)
Neutrinos are perfect probes for the weak force. All other fundamental particles interact through the strong, electromagnetic or weak force or through some combination of the three. Neutrinos are the only particles that interact solely though the weak force. This makes neutrinos important for nailing down the details of the weak force.
Neutrinos are really hard to detect. On average, only one neutrino from the sun will interact with a person’s body during his or her lifetime. Since neutrino interactions are so rare, neutrino detectors must be huge. Super Kamiokande in Japan is as tall as Wilson Hall and holds 50,000 tons of ultrapure water. IceCube is buried between 1.5 and 2.5 kilometers under pure and clear ice in Antarctica, instrumenting a full cubic kilometer of ice.
Neutrinos are like chameleons. There are three flavors of neutrinos: electron, muon and tau. As a neutrino travels along, it may switch back and forth between the flavors. These flavor “oscillations” confounded physicists for decades.
Neutrinos of electron flavor linger around electrons. When neutrinos travel through matter, they see dense clouds of electrons. Electron neutrinos will have trouble traversing these dense clouds, effectively slowing down while muon and tau flavors travel through unimpeded. The NOvA experiment is using this phenomenon to deduce more information about the neutrino masses.
Neutrinos let us see inside the sun. The light that reaches Earth takes 10,000 to 100,000 years to escape the thick plasma of the sun’s core. When light reaches the solar surface, it freely streams through open space to our planet in only 8 minutes. Neutrinos provide us a penetrating view into the core, where nuclear fusion powers the sun. They take only 3.2 seconds to escape to the solar surface and 8 minutes to reach Earth.
Neutrinos may have altered the course of the universe. Why is everything in the universe made predominantly of matter and not antimatter? Cosmologists think that at the start of the universe there were equal parts of matter and antimatter. Neutrino interactions may have tipped this delicate balance, enabling the formation of galaxies, stars and planets like our own Earth.
Neutrinos dissipate more than 99 percent of a supernova’s energy. Certain types of stellar explosions lose nearly all of their energy through neutrinos. These “core collapse” supernovae end as either a black hole or a neutron star. Neutrinos are used to understand how supernovae explode and tell us more about other astronomical objects like active galactic nuclei.
Why wasn’t friendship as good as a relationship? Why wasn’t it even better? It was two people who remained together, day after day, bound not by sex or physical attraction or money or children or property, but only by the shared agreement to keep going, the mutual dedication to a union that could never be codified.
According to the theory of relativity space is not static. The movements of objects can change the structure of space.
In Einstein’s view, space is combined with another dimension - time - which creates universewide “fabric” called space-time. Object travel through this fabric, which can be warped, bent and twisted by the masses and motions of objects within space-time.
One prediction of general relativity was that light should not travel in a perfectly straight line. When traveling through space-time and approaching the gravitational field of a mass object, the light must bend-but not too much.
Then the English astronomer Sir Frank Watson Dyson proposed that the total solar eclipse of 1919 could prove, because the Sun would cross the
bright Hyades star cluster. Star light would have to cross the gravitational field of the sun on the way to Earth, but would be visible due to the darkness of the eclipse. This would allow precise measurements of the positions displaced by the gravity of the stars in the sky.
Because of this, teams of researchers strategically positioned themselves in two locations that would initially provide the best conditions for observing the eclipse. One group stayed in Ilha do Príncipe, in São Tomé and Príncipe, and other researchers settled in Sobral, Ceará (Brazil).
Eddington, who led the experiment, first measured the “true” positions of the stars during January and February of 1919. In May, he went to remote Prince Island (in the Gulf of Guinea, on the west coast of Africa) to measure Positions of the stars during the eclipse, seen through the gravitational lens of the sun.
The total eclipse lasted about 6 minutes and 51 seconds, during those few minutes the astronomers captured several photos of the total eclipse.
When Eddington returned to England, his data from Príncipe confirmed Einstein’s predictions.
Eddington announced his discoveries on November 6, 1919.
3°Image:
Negative of the 1919 solar eclipse taken from the report of Sir Arthur Eddington on the expedition to verify Einstein’s prediction of the bending of light around the sun.
