Answer:
4 days
either multiply 128 by .5 until you get to 2 counting each time or use 2 formulas ln(n2/n1)=-k(t2-t1) to get k then input k into ln(2)=k*t1/2
n2 is final amount and n1 is beginning and t is either time elapsed as in the first formula or the actual half life that is t1/2
Explanation:
Answer:
Final velocity at the top of the ramp is 6.58m/s
Explanation
Check the attachment
Russia shut off the Nord Stream pipeline that supplies natural gas to Germany.
What is the Nord Stream pipeline?
A pair of offshore natural gas pipeline systems in Europe called Nord Stream cross the Baltic Sea from Russia to Germany. It consists of the Nord Stream 1 and Nord Stream 2 pipelines, both of which originate in northwest Russia, near Finland, in Vyborg and Ust-Luga, respectively. Both pipelines travel to Lubmin in the Mecklenburg-Vorpommern state of northeastern Germany.
Due to Russia's invasion of Ukraine, certification for Nord Stream 2 has been rejected. When referring to a larger network of pipelines, such as the feeding onshore pipeline in Russia and additional connections in Western Europe, the term "Nord Stream" is sometimes used.
Nord Stream joins the NEL pipeline to Rehden near Bremen in northwestern Germany and the OPAL pipeline to Olbernhau in eastern Germany at the Czech border in Lubmin.
Thus, the Nord Stream pipeline supplies natural gas to Germany.
Learn more about the natural gas pipeline here,
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P U S S Y
<span>Joy is planning to purchase a sweater that costs $30 dollars at her local department store. The sweaters are on sale for 20% off. Which steps are needed to find the sale price of the sweater?</span>
Great Question! I happened to be a physics nerd!
Answer:
C. Two hydrogen nuclei, each with only one proton, fuse to form deuterium, a form of hydrogen with one proton.
MAKE SURE TO SEE EXPLANATION!
Explanation:
In the core of the Sun, or any other main sequence star, there is no single fusion process. Instead, complex sequences of processes occur to make helium nuclei from hydrogen nuclei (i.e. protons). The proton-proton chain provides for the majority of energy generation in stars with masses less than that of the Sun. One difficulty in creating a helium nucleus (two protons and two neutrons) is that there are only protons to begin with. Some protons must be turned into neutrons in some way. The first step is to combine two protons to form a deuterium nucleus (also known as a deuteron). That's a hefty hydrogen nucleus with one proton and one neutron. Such a proton-proton contact is highly unlikely, and it has never been detected in a laboratory. Fortunately, the Sun's core is incredibly hot and dense, with an incredible number of protons packed inside. Even a low likelihood event will occur every now and again. Along with each deuteron, a positron (an "anti-electron") and a neutrino are created. Because the Sun's core is plasma, there are a lot of free electrons, thus the positron doesn't live long until it and an electron collide and annihilate, resulting in gamma radiation. The deuteron then interacts with a proton to form a helium 3 nucleus. That is a high-probability interaction, and it occurs swiftly. Two helium 3 nuclei join in the third phase to generate a helium 4 ("regular" helium) nucleus and a proton. Branch I of the proton-proton (p-p) chain is responsible for this. Another stage is required because reactions between helium 3 and helium 4 nuclei are possible. There are two conceivable reactions (named Branch II and Branch III), and I'll save you the gory details. It gets much more complicated since theoretical calculations indicate that a reaction between a helium 3 nucleus and a proton is feasible — Branch IV. This reaction has an incredibly low likelihood of occurring, far lower than the Branch I reaction, thus it must be exceedingly rare. The Carbon-Nitrogen-Oxygen (CNO) Cycle is another method for reducing hydrogen to helium. It does not generate much energy in the Sun, but it is the principal energy generation mechanism in larger stars.
