Astrophysical jet caught in a 'speed trap'

SS 433 is a binary star system in which a black hole, with a mass approximately ten times that of the Sun, and a star, with a similar mass but occupying a much larger volume, orbit each other with a period of 13 days. The intense gravitational field of the black hole rips material from the surface of the star, which accumulates in a hot gas disk that feeds the black hole. As matter falls in toward the black hole, two collimated jets of charged particles (plasma) are launched, perpendicular to the plane of the disk, at a quarter of the speed of light.

The jets of SS433 can be detected in the radio to x-ray ranges out to a distance of less than one light year either side of the central binary star, before they become too dim to be seen. Yet surprisingly, at around 75 light-years distance from their launch site, the jets are seen to abruptly reappear as bright X-ray sources. The reasons for this reappearance have long been poorly understood.

Similar relativistic jets are also observed emanating from the centers of active galaxies (for example quasars), though these jets are much larger in size than the galactic jets of SS 433. Due to this analogy, objects like SS 433 are classified as microquasars.

Until recently, no gamma ray emission has ever been detected from a microquasar. But this changed in 2018, when the High Altitude Water Cherenkov Gamma-ray Observatory (HAWC), for the first time, succeeded in detecting very-high-energy gamma rays from the jets of SS 433. This means that somewhere in the jets particles are accelerated to extreme energies. Despite decades of research, it is still unclear how or where particles are accelerated within astrophysical jets.

The study of gamma-ray emission from microquasars provides one crucial advantage: while the jets of SS 433 are 50 times smaller than those of the closest active galaxy (Centaurus A), SS 433 is located inside the Milky Way a thousand times closer to Earth. As a consequence, the apparent size of the jets of SS 433 in the sky is much larger and thus their properties are easier to study with the current generation of gamma-ray telescopes.

Prompted by the HAWC detection, the H.E.S.S. Observatory initiated an observation campaign of the SS 433 system. This campaign resulted in around 200 hours of data and a clear detection of gamma-ray emission from the jets of SS 433. The superior angular resolution of the H.E.S.S. telescopes in comparison to earlier measurements allowed the researchers to pinpoint the origin of the gamma-ray emission within the jets for the first time, yielding intriguing results:

While no gamma-ray emission is detected from the central binary region, emission abruptly appears in the outer jets at a distance of about 75 light years either side of the binary star, in accordance to previous X-ray observations.

However, what surprised the astronomers most, was a shift in the position of the gamma-ray emission when viewed at different energies.

The gamma-ray photons with the highest energies of more than 10 teraelectron-volts, are only detected at the point where the jets abruptly reappear (see fig 2c). By contrast, the regions emitting gamma rays with lower energies appear further along each jet.

"This is the first-ever observation of energy-dependent morphology in the gamma-ray emission of an astrophysical jet," remarks Laura Olivera-Nieto, from the Max-Planck-Institut für Kernphysik in Heidelberg, who was leading the H.E.S.S. study of SS 433 as part of her doctoral thesis. "We were initially puzzled by these findings. The concentration of such high energy photons at the sites of the X-ray jets' reappearance means efficient particle acceleration must be taking place there, which was not expected."

The scientists did a simulation of the observed energy-dependence of the gammy-ray emission and were able to achieve the first-ever estimate of the velocity of the outer jets. The difference between this velocity and the one with which the jets are launched suggests that the mechanism which accelerated the particles further out is a strong shock- a sharp transition in the properties of the medium. The presence of a shock would then also provide a natural explanation for the x-ray reappearance of the jets, as accelerated electrons also produce x-ray radiation.

"When these fast particles then collide with a light particle (photon), they transfer part of their energy -- which is how they produce the high-energy gamma photons observed with H.E.S.S. This process is called the inverse Compton effect," explains Brian Reville, group leader of the Astrophysical Plasma Theory group at the Max Planck Institute for Nuclear Physics in Heidelberg.

"There has been a great deal of speculation about the occurrence of particle acceleration in this unique system -- not anymore: the H.E.S.S. result really pins down the site of acceleration, the nature of the accelerated particles, and allows us to probe the motion of the large-scale jets launched by the black hole" points-out Jim Hinton, Director of the Max Planck Institute for Nuclear Physics in Heidelberg and Head of the Non-thermal Astrophysics Department.

"Just a few years ago, it was unthinkable that ground-based gamma-ray measurements could provide information about the internal dynamics of such a system" adds coauthor Michelle Tsirou, a postdoctoral researcher at DESY Zeuthen.

However, nothing is known about the origin of the shocks at the sites where the jet reappears. "We still don't have a model that can uniformly explain all the properties of the jet, as no model has yet predicted this feature" explains Olivera-Nieto. She wants to devote herself to this task next -- a worthwhile goal, as the relative proximity of SS 433 to Earth offers a unique opportunity to study the occurrence of particle acceleration in relativistic jets. It is hoped that the results can be transferred to the thousand-times larger jets of active galaxies and quasars, which would help solve the many puzzles concerning the origin of the most energetic cosmic rays.

The H.E.S.S. Observatory

High-energy gamma rays can only be observed from the ground with a trick. When a gamma ray enters the atmosphere, it collides with atoms and molecules and generates new particles that race on towards the ground like an avalanche. These particles emit flashes lasting only a few billionths of a second (Cherenkov radiation), which can be observed with specially equipped large telescopes on the ground. High-energy gamma astronomy therefore uses the atmosphere like a giant fluorescent screen. The H.E.S.S. observatory, located in the Khomas Highlands of Namibia at an altitude of 1835m, officially went into operation in 2002. It consists of an array of five telescopes. Four telescopes with mirror diameters of 12 m are located at the corners of a square, with a further 28 m telescope in the center. This makes it possible to detect cosmic gamma radiation in the range of a few tens of gigaelectronvolts (GeV, 10⁹ electronvolts) to a few tens of teraelectronvolts (TeV, 10¹² electronvolts). For comparison: visible light particles have energies of two to three electron volts. H.E.S.S. is currently the only instrument that observes the southern sky in high-energy gamma light and is also the largest and most sensitive telescope system of its kind.