न्यूट्रॉन-तारा हिंदी उपयोग और उदाहरण

आर॰ऍक्स॰ जे१८५६.५-३७५४ (RX J1856.5-3754) - यह एक न्यूट्रॉन तारा है।

जब आर्द्रा फटेगा तो इसके पीछे एक २० किमी के व्यास का न्यूट्रॉन तारा रह जाएगा।

इन प्रस्फोटों का स्रोत अज्ञात है लेकिन वैज्ञानिक इसका न्यूट्रॉन तारा, कालाछिद्र या परग्रही बुद्धि होने का दावा करते हैं।

""खगोलशास्त्र न्यूट्रॉन तारा किसी भारी तारे के महानोवा (सुपरनोवा) घटना (प्रकार- २, 1b एवं 1c) के बाद उसके गुरुत्वीय पतन से बना हुआ अवशेष होता है।

माना जाता है के जिन तारों में इतना द्रव्यमान नहीं होता के वे आगे चलकर अपना इंधन ख़त्म हो जाने पर न्यूट्रॉन तारा बन सकें, वे सारे सफ़ेद बौने बन जाते हैं।

न्यूट्रॉन-तारा इसके अंग्रेजी अर्थ का उदाहरण

This device creates a wormhole between two points in space, allowing a neutron star to be dropped into the planet and ignite stellar nuclear fusion.

When Smolin published the theory in 1992, he proposed as a prediction of his theory that no neutron star should exist with a mass of more than 1.

Later this figure was raised to two solar masses following more precise modeling of neutron star interiors by nuclear astrophysicists.

If a more massive neutron star was ever observed, it would show that our universe's natural laws were not tuned for maximal black hole production, because the mass of the strange quark could be retuned to lower the mass threshold for production of a black hole.

Kaus, "A model of neutron star dynamics" Astrophy.

When massive stars explode as supernovas, they leave behind neutron stars and black holes.

Some of these neutron stars and black holes have nearby companion stars, and become powerful sources of X-rays as they pull matter off their companions (also known as ultra and hyperluminous X-ray sources).

This equation entails that photon spheres can only exist in the space surrounding an extremely compact object (a black hole or possibly an "ultracompact" neutron star).

Jay family In astroparticle physics, an Urca process is a reaction which emits a neutrino and which is assumed to take part in cooling processes in neutron stars and white dwarfs.

The direct Urca processes are the simplest neutrino-emitting processes and are thought to be central in the cooling of neutron stars.

Historically, it has been held that these X-rays might be excited by matter originating from the star, from a hot wind or a disk around the star, accreting onto the surface of a degenerate companion, such as a white dwarf or neutron star.

A neutron star could easily power this X-ray flux, but X-ray emission from neutron stars is known to be non-thermal, and thus in apparent variance with the spectral properties.

Most stars that produce supernovae leave behind compact stellar remnants- a neutron star or black hole, typically depending on the mass of the original star.