Outflow or jets are important feature for star-formation region, and are main solution for researchers to explain many key issues in star-formation. Properties, such as morphologies, size, and velocities, of outflows provide fossil records of the mass ejection and, by inference, the mass accretion histories of forming young stars.
X-rays can trace the nearest origin of outflow, and to explore the mechanism of jet production and its collimation. The mechanism is still not clear, although various feedback models of interaction with interstellar medium have been suggested to explain the X-ray emissions.
Recently, a study led by Profs. ZHAO Gang and LIANG Guiyun from the National Astronomical Observatories of the Chinese Academy of Science (NAOC) has reported a laboratory analog for the collision of outflow with dense clouds in Herbig-Haro 248 and starburst galaxy M82.
The results were published in The Astrophysical Journal on February 2.
By using powerful laser facility of Shengguang-II sited at Shanghai, supersonic outflow with velocity of 330 km/s was generated, which is comparable to that in protostellar outflow. This provides an excellent opportunity to investigate the outflow feedback in star-formation region.
For both large-scale astrophysical plasma and small-scale laboratory plasma, the fundamental physical principles are the same. By using scaling law in time, spatial and density, the two plasmas are similar in many aspects. "We can reproduce and investigate the astrophysical phenomenon, as in HH 248 or M82, in laboratory, and further reveal the fundamental physics in astrophysics," said Prof. LIANG Guiyun, first author of the study.
"Through such experiment, we've found a different conclusion that the X-rays in HH 248 are mainly from the outflow material heated by reverse shock, namely Mach disk. It differs from the past understanding that X-rays are from interstellar medium heated by shock," said Prof. LIANG
By a sophistical emission model, they deduced that charge exchange took place in such a laboratory miniature, as in the cases of HH 248 and Cap in M82.
However, there are still some differences after scaling law for the two different systems. A further laboratory exploration is necessary to figure the pictures of outflow interaction in protostars.
