Principle of Subramaniam Chandrasekhar, Chandrasekhar Limit.

The maximum potential mass of a permanent white dwarf constellation is called the Chandrasekhar limit. This limitation was first mentioned in Wilhelm Andersen and E. C. Stoner in his papers published in 1930. But astronomer Subrahmanyan Chandrasekhar of India, in 1930, at the age of 19 years, freely discovered this limit and made the count of this boundary more pure.

At present, the approved value of Chandrasekhar Bound is approximately 1.39 (2.765 × 1030 kg) is.Subramaniam Chandrasekhar renders the theory about the constellations of 'White dwarf', i.e. the 'white dwarf'.

The limit that they have set for these constellations is called 'Chandrasekhar Border'. From his theory, many secrets have been discovered about the origin of the universe. He is very famous for his magnificent 'Chandrasekhar Border'.

He showed that there is a high mass that can be supported against gravity by the pressure made by electrons and atomic nuclei. The value of this limit is approximately 1.44 times the mass of a solar mass. Explain that in his last interview, he had said, "Although I am an atheist Hindu, but when I see it with a logical point of view, I find that God is the greatest and most wonderful invention of God.Indian scientist Subrahmanyam Chandrasekhar is named after the scientist who received the Nobel Prize in Physics in the year 1983. Chandrasekhar Border This is the maximum mass of a static white wave star. After greater masses, the process of breaking the star begins and it turns into a neutron star or black hole later.

Chandrasekhar had estimated this limit at the age of 20. He found the Nobel Prize in Physics for those important discoveries, on the basis of which the theory of 'the post-developmental phase behind heavy masses' was made. Presently this principle is universally acceptable in all the world.

Comments

NASA/ESA Hubble Space Telescope Reveals New Details of the Orion Nebula’s Star Formation.

This NASA/ESA Hubble Space Telescope image captures the Orion Nebula (Messier 42, M42), the nearest star-forming region to Earth, located about 1,500 light-years away. A captivating new image captured by the NASA/ESA Hubble Space Telescope offers an extraordinary look into the Orion Nebula, the nearest massive star-forming region to Earth. Located just 1,500 light-years away, this nebula is visible to the naked eye below the three stars forming Orion's "belt." The region is home to hundreds of newborn stars, including two protostars featured in the image: HOPS 150 and HOPS 153. Named after the Herschel Orion Protostar Survey, conducted with ESA’s Herschel Space Observatory, the protostars HOPS 150 and HOPS 153 provide key insights into the early stages of star formation. HOPS 150, visible in the upper-right corner of the image, is a binary star system, with two young stars orbiting one another. These protostars are surrounded by small dusty disks, where material from th...

New Method Detects Small Asteroids in Main Belt, Offering Insight for Planetary Defense.

An international team of physicists, led by MIT researchers, has developed a groundbreaking method to detect small asteroids, as small as 10 meters in diameter, within the main asteroid belt. These space rocks, ranging from the size of a bus to several stadiums wide, were previously undetectable using traditional methods. The team's discovery, detailed in a paper published in Nature, could significantly improve tracking of potential asteroid impactors, aiding planetary defense efforts. The main asteroid belt, located between Mars and Jupiter, is home to millions of asteroids, but until now, scientists could only detect objects roughly a kilometer in diameter. The new detection technique, which utilizes the "shift and stack" method, is able to identify much smaller asteroids, even those far from Earth, enabling more precise orbital tracking. This breakthrough is crucial for planetary defense, allowing scientists to spot near-Earth objects that may pose a threat in the fu...

XSPECT Payload Successfully Validates Performance through Cas A Observation.

The XSPECT instrument captures a detailed spectrum of the supernova remnant Cassiopeia A (Cas A), encompassing both the Galactic Cosmic Ray (GCR) background and the Cosmic X-ray Background (CXB). The flux observed above 8 keV predominantly results from the combined contributions of CXB and GCR. The presented spectrum, depicted in the figure, is derived from a cumulative integration time of 20 ksec, collected across multiple orbits, providing valuable insights into the X-ray emissions associated with Cas A. XPoSat, India's inaugural X-ray polarimetric mission, has achieved a significant as the XSPECT instrument captures its initial observations from the Cassiopeia A (Cas A) supernova remnant. Launched on January 1, 2024, XPoSat is equipped with two co-aligned instruments, namely the POLarimeter Instrument in X-rays (POLIX) and X-ray SPECtroscopy and Timing (XSPECT). This mission is designed to unravel the mysteries of cosmic X-ray sources. While POLIX focuses on examining X-ray po...

Infinity Cosmos

Search This Blog