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  2. Accretion disk - Wikipedia

    en.wikipedia.org/wiki/Accretion_disk

    An accretion disk is a structure (often a circumstellar disk) formed by diffuse material [a] in orbital motion around a massive central body. The central body is most frequently a star . Friction , uneven irradiance, magnetohydrodynamic effects, and other forces induce instabilities causing orbiting material in the disk to spiral inward toward ...

  3. File:Millisecond pulsar and accretion disk - NASA animation ...

    en.wikipedia.org/wiki/File:Millisecond_pulsar...

    English: Animation showing neutron star and accretion disk evolving into a millisecond pulsar, with magnetic fields. The formation of a pulsar: A star in a binary star system has collapsed to a neutron star. It begins to gain material from its companion star (known as "accretion").

  4. Magnetorotational instability - Wikipedia

    en.wikipedia.org/wiki/Magnetorotational_instability

    The magnetorotational instability (MRI) is a fluid instability that causes an accretion disk orbiting a massive central object to become turbulent.It arises when the angular velocity of a conducting fluid in a magnetic field decreases as the distance from the rotation center increases.

  5. X-ray binary - Wikipedia

    en.wikipedia.org/wiki/X-ray_binary

    The brightest part of the system is the accretion disk around the compact object. The orbital periods of LMXBs range from ten minutes to hundreds of days. The variability of LMXBs are most commonly observed as X-ray bursters, but can sometimes be seen in the form of X-ray pulsars.

  6. Accretion (astrophysics) - Wikipedia

    en.wikipedia.org/wiki/Accretion_(astrophysics)

    In astrophysics, accretion is the accumulation of particles into a massive object by gravitationally attracting more matter, typically gaseous matter, into an accretion disk. [ 1 ] [ 2 ] Most astronomical objects , such as galaxies , stars , and planets , are formed by accretion processes.

  7. Nebular hypothesis - Wikipedia

    en.wikipedia.org/wiki/Nebular_hypothesis

    The disk of a Class 0 protostar is thought to be massive and hot. It is an accretion disk, which feeds the central protostar. [39] [40] The temperature can easily exceed 400 K inside 5 AU and 1,000 K inside 1 AU. [51] The heating of the disk is primarily caused by the viscous dissipation of turbulence in it and by the infall of the gas from the ...

  8. Circumstellar disc - Wikipedia

    en.wikipedia.org/wiki/Circumstellar_disc

    The main accretion phase lasts a few million years, with accretion rates typically between 10 −7 and 10 −9 solar masses per year (rates for typical systems presented in Hartmann et al. [2]). Illustration of the dynamics of a proplyd. The disc gradually cools in what is known as the T Tauri star stage.

  9. List of Adobe software - Wikipedia

    en.wikipedia.org/wiki/List_of_Adobe_software

    Photoshop Album is a piece of application software by Adobe Systems designed to import, organize and edit digital photos, and allows quick and easy searching and sharing of entire photo collections. Prelude was an ingest and logging tool for tagging media with metadata for searching, post-production workflows, and footage lifecycle management ...