Black holes have this incredible ability to literally stretch you into a long spaghetti-like strand. appropriately, this phenomenon is called 'spaghettification'. the way it works has to do with how gravity behaves over distance. right now, your feet are closer to the centre of earth and are therefore more strongly attracted than your head. under extreme gravity, say, near a black hole, that difference in attraction will actually start working against you.
as your feet begin to get stretched by gravity's pull, they will become increasingly more attracted as they inch closer to the centre of the black hole. the closer they get, the faster they move. but the top half of your body is farther away and so is not moving toward the centre as fast. the result: spaghettification!
Do not go gentle into that good night, old age should burn and rave at close of day; rage, rage against the dying of the light. though wise men at their end know dark is right, because their words had forked no lightning they do not go gentle into that good night #interstellar
And here we have 6 helium flashes in the core of some star! it's hard to see in the helium abundance graph--bottom--, but highly evident in the abundance, energy contribution, and mixing plots respectively from the top down. helium flashes occur in shells around inert stellar cores, generating pulses of energy that echo through the star.
Behold! the numerical evolution of a sun like star from birth to death. the top left panel is the one that traces the star's luminosity versus temperature--called an hr diagram--, and indicates what type of star we're looking at at the moment. the main-sequence and sub-giant phases are quick to pass in this video, but the red giant and asymptotic giant branches last the longest, with the simulation terminating abruptly upon the final nova and progression to a white dwarf!
the top right panel indicates the most prevalent energy sources throughout the layers of the star. the most interesting one is the bottom right panel, which shows the abundances of various elements throughout the star at different layers. that's where the magic happens, and the nuclear processes are evident. the bottom left is the temperature-density profile, which tells us what types of fusion are going on, and whether the star is going to b**w itself apart or fail to fuse somewhere.
Ngc 520 (arp 157) is a pair of highly disturbed colliding spiral galaxies about 100,000 light-years across, located some 90.7 million light-years away in the constellation pisces. it has an h ii nucleus, contains a number of radio sources and is a source of infrared radiation. ngc 520 is one of the brightest interacting galaxies in the sky.
two enormous spiral galaxies are crashing into each other, melding and forming a new conglomerate. this happens slowly, over millions of years — the whole process started some 300 million years ago. the object is now in the middle stage of the merging process, as the two nuclei haven’t merged yet, but the two discs have. some astronomers predict that this is the fate that awaits the milky way and the andromeda galaxy (m 31) in about 5 billion years.
ngc 520 shows very obvious tidal features and prominent dust lanes. the merger is giving rise to the enhanced star formation. the primary nucleus has the most elevated star formation activity. the emission and absorption features seen in its spectra are consistent with a very young stellar population.
although the speeds of stars are fast, the distances are so vast that the interacting pair will surely not change its shape noticeably during our lifetimes.
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