Hardik Pandya last over

Read More

BLACK HOLES, BROWNIAN MOTION

BLACK HOLES, BROWNIAN MOTION

If you’ve ever watched dust-motes dancing in a sunbeam then you’ve observed Brownian motion. It is the jerky, fluttering motion of particles in fluids such as air or water. The botanist Robert Brown first described the motion in detail. He demonstrated that it was not caused by some living organism, but was never able to determine its cause. That answer came from Albert Einstein, who proved that Brownian motion was due to molecules of the fluid colliding with the Brownian particle.  Brownian motion was definitive proof of the atomic theory of matter. Even though we couldn’t (at that time) see the atoms which make up matter, we could see the effect of their existence.

What does all this have to do with black holes? Well it turns out black holes also undergo Brownian motion, and astronomers can use that fact to their advantage.

Brownian_motion_large
BROWNIAN MOTION ANIMATION. SOURCE: WIKIMEDIA

Within most galaxies is a supermassive black hole. These typically have a mass a hundred thousand to a billion times larger than our sun. They reside in the center of the galaxy, surrounded by a dense cluster of stars. Just as a dust-mote is knocked about by the tiny atoms surrounding it, the black hole is knocked about by the (relatively) tiny stars surrounding it. Obviously we can’t observe this motion in real time, but its effect is clearly measurable.

There is an important difference between dust-motes and black holes. For traditional Brownian motion, the atoms move very much like billiard balls. An atom moves freely through space until it collides with the dust-mote, the collision happens very quickly, and then the atom moves freely again. But stars surrounding a black hole do not interact like billiard balls. For stars and black holes, the interaction varies depending on how close a star is to the black hole. This means that while the billiard-ball type model for Brownian motion can’t be used to model stars and black holes, you also have to take into account how the black hole’s gravity affects the distribution of stars in the first place.

Typically, the Brownian motion of a black hole has been modeled by starting with a galaxy of stars in an equilibrium state, then adding the black hole to the model to see what happens. But fellow RIT faculty David Merritt and his team modeled a galaxy of stars in equilibrium with the central black hole from the beginning. What they were able to show was that this new approach makes a significant difference in your predicted outcomes. Essentially, the presence of the black hole means that closer stars have more kinetic energy on average than more distant stars, and these closer stars in turn create most of the Brownian motion of the black hole.

The reason this matters is that Brownian motion can be used to determine the mass of the black hole in the center of our Milky Way galaxy. Measure the distribution of stellar speeds near the center of our galaxy and you can determine the mass of the central black hole. Merritt and co. determined the mass of our galactic black hole to be about 1.2 million solar masses. Pretty big, but smaller than older measurements which gave a value of about 3 million solar masses.

All this from treating a huge black hole as a cosmic speck of dust.

Read More

Sandeep Maheshwari Inspirational speech over life & Opportunity

Life always have opportunities......

Find it....
Never Give up...........

Read More

Intelligent Story: The Genius Einstein's Driver

There is a story about how Albert Einstein was traveling to universities, giving lectures on his famous theory of relativity. One day while on their way to a university,

The driver said:" Dr. Einstein, I've heard that lecture more than 30 times. I have learned it by heart and bet I could give it myself."

"Well, I'll give you the chance," said Einstein,

"They don't know me at the next school, so when we get there I'll put on your cap and you introduce yourself as me and give the lecture." Einstein continued.

At the hall, the driver gave Einstein's lecture so wonderfully that he didn't make any mistakes.

When he finished, he started to leave, but one of the professors stopped him and asked him a question which was very difficult. The aim of the question was not gaining knowledge but embarrassing Einstein.

The driver thought fast.

"The answer to that problem is so simple," he said,

"I'm surprised you have to ask me. In fact, to show you just how simple it is, I'm going to ask my driver to come up here and answer your question."!

Then Einstein stood up and gave an incredible answer to the question of that professor.

~ Moral of the story: No matter how genius you pretend to be, there is always someone who is more genius than you despite his position.

Read More

Something You Need To Know About Your Blood Group.

Something You Need To Know About Your Blood Group.

Whats Your Type And How Common Is It?





O+  1 in 3    (37.4%) (Most common)
A+  1 in 312  (35.7%)
B+  1 in 1229 (8.5%)
AB+ 1 in 2915 (3.4%)
O-  1 in 1516 (6.6%)
A-  1 in 16   (6.3%)
B-  1 in 67   (1.5%)
AB- 1 in 167  (.6%) (Rarest)




Compatible Blood Types




O-  Can Receive O-
O+  Can Receive O+ O-
A-  Can Receive A- O-
A+  Can Receive A+ A- O+ O-
B-  Can Receive B- O-
B+  Can Receive B+ B- O+ O-
AB- Can Receive AB- A- B- O-
AB+ Can Receive AB+ AB- A- B- A+ B+ O- O+






This is an important information which can save life! Please share with more and more people.

Read More

Work untill ur idol becoms ur rivel....

Read More

What are Gravitational Waves?

Today, the National Science Foundation (NSF) announced the detection of gravitational waves by the Laser Interferometer Gravitational-Wave Observatory (LIGO), a pair of ground-based observatories. But…what are gravitational waves? 

Let us explain:

Gravitational waves are disturbances in space-time, the very fabric of the universe, that travel at the speed of light. The waves are emitted by any mass that is changing speed or direction. The simplest example is a binary system, where a pair of stars or compact objects (like black holes) orbit their common center of mass.

We can think of gravitational effects as curvatures in space-time. Earth’s gravity is constant and produces a static curve in space-time. A gravitational wave is a curvature that moves through space-time much like a water wave moves across the surface of a lake. It is generated only when masses are speeding up, slowing down or changing direction.

Did you know Earth also gives off gravitational waves? Earth orbits the sun, which means its direction is always changing, so it does generate gravitational waves, although extremely weak and faint.

What do we learn from these waves?

Observing gravitational waves would be a huge step forward in our understanding of the evolution of the universe, and how large-scale structures, like galaxies and galaxy clusters, are formed.

Gravitational waves can travel across the universe without being impeded by intervening dust and gas. These waves could also provide information about massive objects, such as black holes, that do not themselves emit light and would be undetectable with traditional telescopes.

Just as we need both ground-based and space-based optical telescopes, we need both kinds of gravitational wave observatories to study different wavelengths. Each type compliments the other.

Ground-based: For optical telescopes, Earth’s atmosphere prevents some wavelengths from reaching the ground and distorts the light that does.

Space-based: Telescopes in space have a clear, steady view. That said, telescopes on the ground can be much larger than anything ever launched into space, so they can capture more light from faint objects.

How does this relate to Einstein’s theory of relativity?

The direct detection of gravitational waves is the last major prediction of Einstein’s theory to be proven. Direct detection of these waves will allow scientists to test specific predictions of the theory under conditions that have not been observed to date, such as in very strong gravitational fields.

In everyday language, “theory” means something different than it does to scientists. For scientists, the word refers to a system of ideas that explains observations and experimental results through independent general principles. Isaac Newton’s theory of gravity has limitations we can measure by, say, long-term observations of the motion of the planet Mercury. Einstein’s relativity theory explains these and other measurements. We recognize that Newton’s theory is incomplete when we make sufficiently sensitive measurements. This is likely also true for relativity, and gravitational waves may help us understand where it becomes incomplete.

Read More

GALILEO – ΒULLET / MISSILE THEORY

*** GALILEO – ΒULLET / MISSILE THEORY - NEWTON : if you shoot (horizontally and straight to the target) with a gun G3 kneeling or lying a target at 300 meters, given that the bullet runs with 800 m / sec , at 1/3 sec the bullet goes to the center of the target and it has not gone down (having a greater range). (I've done it personally hitting the center of the target with 10 continious bullets). If you leave it from the same small height it takes again 1/3 sec the most to reach the ground. (The same happens to a space without air -air resistance- , except that there the target must be put a little farther or a little closer than 300 meters since the speed changes a little). Thus the Galileo proposal that a body that is pushed horizontally will fall to the ground at the same time with a body that is vertically left to fall at the same time from the same height , is not exactly correct but it is quite statistic and has to do with a rather weak push. Further on the basis of Galileo – Newton , in the fall of bodies, the vertical distance is proportional (analogic) to the square of the time since Galileo let objects to fall to the ground from a ski slope : when the body left the ski slope it traveled a horizontal distance (the shadow of which in the ground is the time of the drop) , and also it traveled a vertical distance (which is the distance between the edge of the ski slope and the ground) and this distance is the space of the fall. However , if we select a different – bigger ski slope with much larger vertical length (in the same distance from the ground as before) we shall see that the horizontal vector-time-shadow will be bigger than before because the body in the ski slope has taken much more speed than before. So the analogy is rather ruined. Therefore we see that the physics of proposals (calculus Principia propositions) of Galileo - Newton (F = G mM / r2 , etc.) is a good and reasonable statistical technical approach that weakens in bigger conditions. THE TRUE MAN IS THE MEASURE OF ALL FLUID THINGS.

*** ΑΒΟUT THE ACCELERATION ¨ further , simply put , Galileo's acceleration a =S/t2 means that '' a body moves with eg 4 m/1sec2 '' (ie 1 sec squared). This means that '' the body in 1 sec is moving at 4 m/sec '' or that '' in the end of 1 sec the body covers 4 m in 1 sec i.e. 0,4 min 0,1 sec as momentum speed''. However (since as we said if we choose another Galileo ski slope the Galileo square analogy in time would not be exactly correct) -since the momentum ιnstantaneous speed is fluid , it could be said that : '' at the end of 1 sec the body covers 0 ,4 m in 0.1 sec at the end of which 0.1 sec the body covers 0,04 m in 0,01 sec '' and the acceleration could be defined as a =S/t3 ie 4m/1sec3 (ie sec cubed and not squared). Thus other equations should also be changed. Eg the equation of Galileo for the ''average speed' of an accelerated body S =(1/2)at2 has to do not only with the acceleration of gravity ''G = 9,8 m / sec2'' but also with any other acceleration even larger , so it also could be cubed instead of squared. (Even if we accept the Galileo square , the truth is that a falling accelarating body does not easily accept a definition of a stable ''average speed'' 5m / sec , because if in the first sec it has traveled 5 m, in the 2nd sec it will have traveled much greater distance , for example at least 20 m. And if we put the cube in the acceleration equation it would be even bigger with obvious consequences in the Newtonian ''F = GmM/r2''. So we are talking about rather fluid and calculus type equations that do not involve much wider and bigger conditions.

Trully if you accept ''average speed'' 5m/sec = in 1 sec 5 m , you cannot easilly accept ''average speed'' 20m/2 sec=10m/sec=in 1 sec 10 m , so it is all statistic and fluid.

-------------------------------------------------------------------------------------------------------------------------------------------------

In this post i mean 9,8 = g and not G

-------------------------------------------------------------------------------------------------------------------------------------------------

Read More

On the deceleration or acceleration

Further, in simple terms under acceleration a galilean =s / T2 means '' A body moving bc with 4 M / 1 Sec2 '' (i.e. 1 Sec Squared). That means '' The body in 1 SEC IS MOVING AT 4 M / SEC '' So how '' At the end of a sec body cover 4 M IN 1 sec i.e. 0,4 m in 0,1 sec ''. However (since like we said, if you choose more galilaiikḗ slide would be undermined as a statistical the proportion of the block) Here-because the instant speed is fluid concept-could have said this: '' At the end of a sec body cover 0,4 m in 0,1 sec at the end of which 0,1 sec body cover 0,04 m in 0,01 SEC '' And Set the acceleration as a =s / t3 i.e. 4 M / sec sec3 (i.e. in the cube-and not on the block). It should be amended and other similar types. Bc the-Average-type of Galileo for '' Average speed '' A body of accelerating χ=(at2 1/2) not only for the acceleration of gravity '' G = 9,8 m / sec2 '' But every other acceleration however big, so I'll epidécheto and power in the cube instead of power on the block. (besides-even if we accept the block of Galileo-a falling body accelerating cannot be easily definition fixed medium speed bc steady speed on average 5 M / sec, because if the first sec has comes 5 M, in 2 O sec will have travelled far greater distance bc at least 20 m. If we put cube the acceleration would be even greater with obvious consequences in Newton '' F=Gmm / R2 ''. Basically it is a largely types these weekly meetings, autoanaphorikoús, by way of trigon not relating to much broader conditions.

*** ΑΒΟUT THE ACCELERATION AND GALILEO : further , simply put , Galileo's acceleration a =S/t2 means that '' a body moves with eg 4 m/1sec2 '' (ie 1 sec squared). This means that '' the body in 1 sec is moving at 4 m/sec '' or that '' in the end of 1 sec the body covers 4 m in 1 sec i.e. 0,4 m in 0,1 sec as momentum speed''. However (since as we said if we choose another Galileo ski slope the Galileo square analogy in time would not be exactly correct) -since the momentum ιnstantaneous speed is fluid , it could be said that : '' at the end of 1 sec the body covers 0 ,4 m in 0.1 sec at the end of which 0.1 sec the body covers 0,04 m in 0,01 sec '' and the acceleration could be defined as a =S/t3 ie 4m/1sec3 (ie sec cubed and not squared). Thus other equations should also be changed. Eg the equation of Galileo for the ''average speed' of an accelerated body X =(1/2)at2 has to do not only with the acceleration of gravity ''G = 9,8 m / sec2'' but also with any other acceleration even larger , so it also could be cubed instead of squared. (Even if we accept the Galileo square , the truth is that a falling accelarating body does not easily accept a definition of a stable ''average speed'' 5m / sec , because if in the first sec it has traveled 5 m, in the 2nd sec it will have traveled much greater distance , for example at least 20 m. And if we put the cube in the acceleration equation it would be even bigger with obvious consequences in the Newtonian ''F = GmM/r2''. So we are talking about rather fluid and calculus type equations that do not involve much wider and bigger conditions.

Trully if you accept ''average speed'' 5m/sec = in 1 sec 5 m , you cannot easilly accept ''average speed'' 20m/2 sec=10m/sec=in 1 sec 10 m , so it is all statistic and fluid.
The most famous guy for straight smooth movement is the u =S / T. The guy who gave himself Galileo to express the average speed of an accelerated college is x = (1/2) a t2, whom I have. As I mentioned the guy under the galilean concerns expression of the average speed of an accelerated college and no rectilinear smooth movement (U= s / T) neither of the acceleration (a =S / T2). If in a mean in acceleration put the g so the acceleration due to gravity 9,8 m / sec2, we get 5 M IN 1 SEC AND 20 M IN 2 sec so we have an expression of the average speed for A falling body as follows: average speed of 5 M IN 1 sec and average speed of 20 metres in 2 sec and average speed of 45 M IN 3 SEC, etc.

Read More