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Черная дыра

Микроквазар

SS433

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For many a century mankind has striven to understand what space is made of.

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And if a measly hundred years ago this information was confined exclusively to theory,

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today thanks to advanced telescopes we are able to see many parts of the universe around us for the first time.

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As the picture of the closest areas of space gained in detail,

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the observer would again and again invariably encounter phenomena whose nature would prove to be harder to identify.

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Many of these are still able to leave the entire scientific community at a loss.

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For example, imagine one of the most exotic and bizarre objects in the universe…

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A celestial body previously unknown to science.

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A binary system spewing out jets of matter at a speed reaching ¼ of the speed of light.

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This is a microquasar dubbed SS 433.

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As a rule, microquasars are X-ray binaries, that is, stellar systems made up of 2 components.

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One of them is a regular star similar to our Sun.

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The other component is a compact object like a black hole or a neutron star.

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Matter in such microquasars is constantly in the process of accumulating in the compact object,

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which is accompanied by occasional outflows of matter at great speeds.

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These outflows are known as jets and the nature of these jets reminds one of processes taking place in regular quasars.

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Now, it is not a regular occurrence in ordinary quasars.

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Meanwhile, as the mass of a microquasar is smaller than that of an ordinary quasar,

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jets may originate here practically on a daily basis.

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The principal difference between microquasars and ordinary quasars is in their mass and the frequency of matter ejections.

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For example, the mass of the compact components in microquasars is considerably smaller

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than the mass of those in regular quasars – it is just several solar masses.

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Just to compare – the average mass of a supermassive black hole in the centre of a quasar may be approximately as much

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as 100,000,000 solar masses.

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As for the mass of the black hole likely to be found in the centre of SS 433, it must be just a few dozen solar masses.

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The accretion disc of a microquasar is intensely luminescent, with emissions in the optical and X-ray bands.

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A regular quasar is an astronomical body boasting the highest luminosity among other objects in the observable universe.

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According to contemporary scientific views,

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these celestial bodies are active cores of galaxies where a supermassive black hole sucks in matter all around it

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thus forming an accretion disc.

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As for the disc itself, it is a source of very powerful luminosity.

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Just to give you an idea – its luminosity may sometimes be hundreds of times as intense as that of all stars in a galaxy like ours combined.

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To date, over 200,000 quasars have been identified.

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We are able to observe some of these quasars in the sky even without using a telescope.

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And so the rate of discovering new objects of one or the other category is another principal parametre

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by which regular quasars and microquasars differ:

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if we look the list of known microquasars, it contains just a few entries so far.

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The first microquasar was discovered back in 1978

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when a source of unusual radio and X-ray emissions was detected by two astronomers

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from the University of Cambridge as they were looking for debris left over from supernovae.

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Detected in the constellation Aquila, this source was later dubbed SS-433.

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The object under scrutiny is an eclipsing X-ray binary system.

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One of its components is likely to be a black hole.

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As for the second component, it is a star of spectral type A.

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That is, a main sequence dwarf star of a whitish hue.

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It is assumed that this star’s mass is 10-30 times that of our Sun.

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And more likely than not, the dwarf used to be considerably heavier in the earlier stages of its existence.

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Its surface temperature is thought to be anything from 7,000 to 11,500 degrees Kelvin.

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This temperature range is typical for stars of this type.

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It is its temperature that gives the star its pale yellow tint.

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In fact, if we look at the stars closest to the Sun, then Sirius, Altair and Vega fall into the same class as this star.

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SS 433 is located within the supernova remnant W50 sometimes also called the Manatee Nebula.

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The age of this nebula is estimated at approximately 20,000 years

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and the distance between the nebula and the Earth measures about 18,000 light years.

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The jets from SS 433 distort the clouds surrounding the W50 nebula.

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According to a certain theory, the W50 Nebula and the microquasar SS 433 are actually related

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and came to be as a result of one and the same supernova event which supposedly took place around 20,000 years ago.

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It takes either of the two objects in the system 13.1 days to orbit the common mass centre.

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In fact, the way the SS 433 system works is quite exciting, with both components constantly interacting with each other.

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Matter from the second component – that is, the regular star – flows to the first component, or the primary,

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supposedly a black hole, thus forming an accretion disc around it.

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As it spirals, the matter heats up to extreme temperatures and emits X-rays.

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Some part of this matter leaves the system in two jets at the rate of approximately 26% of the speed of light –

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that is, 79,000 km per second.

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In 2019, thanks to the ALMA observatory, astronomers managed to get detailed images of SS 433.

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It was clear from the emission structure

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that the microquasar’s jets themselves are rather narrow and their shape is irregular and has nodes.

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Further studies of the object showed that the shape of the jets is distorted as a result of precession –

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that is, a process when the jets slowly rotate on their axis as they spiral.

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The diametre of either of the two jets ejected from the microquasar in two opposite directions measures approximately

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5,000 times the diametre of the Solar System.

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As SS 433 is relatively close to the Earth,

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it is particularly valuable to scientists studying the phenomenon of microquasars.

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Images beamed back by the ALMA Observatory showed its jets for the first time.

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And it also helped establish that the direction these jets point at is never the same –

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just like a top, the spinning toy, gradually slows down, they, too, rotate on their axis

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which is perpendicular to the plane of the accretion disc.

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The ALMA images boasted another outstanding feature:

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the shape of SS 433 was predicted in fine detail thanks to spectroscopic measurements

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that had been done in 2018 using the Global Jet Watch telescopes.

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And so the actual shape largely corresponds to the new images

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where SS 433 is really seen to have a shape reminding one of a corkscrew.

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It isn’t a rare occasion when jets like that originate here or there in the universe.

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As a rule, jets of plasma, also known as relativistic jets,

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are spewed out of the centres of active galaxies, quasars and radio galaxies.

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When this occurs, there are usually two jets as such pointing in the opposite directions.

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And this is exactly what we can observe in the case of SS 433.

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Today the phenomenon of jets like that wants deeper studying.

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It is believed that jets originate following the interaction between magnetic fields

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and the accretion disc around a black hole or a neutron star.

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As for their size, it may be staggeringly enormous.

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In the case of the radio galaxy 3C 120, for example,

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the jet stretches for at least several kiloparsecs away from its source.

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It is highly probable that in the future the regular star in the SS 433 system

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will shed its outer layer completely as a result of the influence of the compact object.

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Its core, meanwhile, will remain hot, and thus the star will qualify to be called a hot subdwarf.

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Later the star is to be gradually sucked in by the black hole

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and sooner or later, after this process is completed, the SS 433 system will assume a classical look –

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it will comprise just the compact object.

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The process of this system’s evolution will of course continue for thousands of years,

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so we have plenty of time to study this phenomenon!

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And while the microquasar SS 433 is active,

00:10:30

we will have many opportunities to carry out detailed observation

00:10:34

that would help us understand the nature of this celestial object!

00:10:37

Let’s keep in touch!

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