image: This artist’s impression shows the pulsar PSR J1023+0038 stealing gas from its companion star. This gas accumulates in a disc around the pulsar, slowly falls towards it, and is eventually expelled in a narrow jet. In addition, there is a wind of particles blowing away from the pulsar, represented here by a cloud of very small dots. This wind clashes with the infalling gas, heating it up and making the system glow brightly in X-rays and ultraviolet and visible light. Eventually, blobs of this hot gas are expelled along the jet, and the pulsar returns to the initial, fainter state, repeating the cycle. This pulsar has been observed to switch incessantly between these two states every few seconds or minutes. view more
Credit: ESO/M. Kornmesser
With a remarkable observational campaign that involved 12 telescopes both on the ground and in space, including three European Southern Observatory (ESO) facilities, astronomers have uncovered the strange behaviour of a pulsar, a super-fast-spinning dead star. This mysterious object is known to switch between two brightness modes almost constantly, something that until now has been an enigma. But astronomers have now found that sudden ejections of matter from the pulsar over very short periods are responsible for the peculiar switches.
“We have witnessed extraordinary cosmic events where enormous amounts of matter, similar to cosmic cannonballs, are launched into space within a very brief time span of tens of seconds from a small, dense celestial object rotating at incredibly high speeds,” says Maria Cristina Baglio, researcher at New York University Abu Dhabi, affiliated with the Italian National Institute for Astrophysics (INAF), and the lead author of the paper published today in Astronomy & Astrophysics.
A pulsar is a fast-rotating, magnetic, dead star that emits a beam of electromagnetic radiation into space. As it rotates, this beam sweeps across the cosmos — much like a lighthouse beam scanning its surroundings — and is detected by astronomers as it intersects the line of sight to Earth. This makes the star appear to pulse in brightness as seen from our planet.
PSR J1023+0038, or J1023 for short, is a special type of pulsar with a bizarre behaviour. Located about 4500 light-years away in the Sextans constellation, it closely orbits another star. Over the past decade, the pulsar has been actively pulling matter off this companion, which accumulates in a disc around the pulsar and slowly falls towards it.
Since this process of accumulating matter began, the sweeping beam virtually vanished and the pulsar started incessantly switching between two modes. In the ‘high’ mode, the pulsar gives off bright X-rays, ultraviolet and visible light, while in the ‘low’ mode it’s dimmer at these frequencies and emits more radio waves. The pulsar can stay in each mode for several seconds or minutes, and then switch to the other mode in just a few seconds. This switching has thus far puzzled astronomers.
"Our unprecedented observing campaign to understand this pulsar’s behaviour involved a dozen cutting-edge ground-based and space-borne telescopes," says Francesco Coti Zelati, a researcher at the Institute of Space Sciences, Barcelona, Spain, and co-lead author of the paper. The campaign included ESO’s Very Large Telescope (VLT) and ESO’s New Technology Telescope (NTT), which detected visible and near-infrared light, as well as the Atacama Large Millimeter/submillimeter Array (ALMA), in which ESO is a partner. Over two nights in June 2021, they observed the system make over 280 switches between its high and low modes.
“We have discovered that the mode switching stems from an intricate interplay between the pulsar wind, a flow of high-energy particles blowing away from the pulsar, and matter flowing towards the pulsar,” says Coti Zelati, who is also affiliated with INAF.
In the low mode, matter flowing towards the pulsar is expelled in a narrow jet perpendicular to the disc. Gradually, this matter accumulates closer and closer to the pulsar and, as this happens, it is hit by the wind blowing from the pulsating star, causing the matter to heat up. The system is now in a high mode, glowing brightly in the X-ray, ultraviolet and visible light. Eventually, blobs of this hot matter are removed by the pulsar via the jet. With less hot matter in the disc, the system glows less brightly, switching back into the low mode.
While this discovery has unlocked the mystery of J1023’s strange behaviour, astronomers still have much to learn from studying this unique system and ESO’s telescopes will continue to help astronomers observe this peculiar pulsar. In particular, ESO’s Extremely Large Telescope (ELT), currently under construction in Chile, will offer an unprecedented view of J1023’s switching mechanisms. “The ELT will allow us to gain key insights into how the abundance, distribution, dynamics, and energetics of the inflowing matter around the pulsar are affected by the mode switching behavior,” concludes Sergio Campana, Research Director at the INAF Brera Observatory and coauthor of the study.
More information
This research was presented in a paper to appear in Astronomy & Astrophysics (doi:10.1051/0004-6361/202346418)
The team is composed of M. C. Baglio (Center for Astro, Particle, and Planetary Physics, New York University Abu Dhabi, UAE [NYU Abu Dhabi]; INAF – Osservatorio Astronomico di Brera, Merate, Italy [INAF Brera]), F. Coti Zelati (Institute of Space Sciences, Campus UAB, Barcelona, Spain [ICE–CSIC]; Institut d’Estudis Espacials de Catalunya (IEEC), Barcelona, Spain [IEEC]; INAF Brera), S. Campana (INAF Brera), G. Busquet (Departament de Física Quànticai Astrofísica, Universitat de Barcelona, Spain; Institut de Ciències del Cosmos, Universitat de Barcelona, Spain; IEEC), P. D’Avanzo (INAF Brera), S. Giarratana (INAF – Istituto di Radioastronomia, Bologna, Italy [INAF Bologna]; Department of Physics and Astronomy, University of Bologna, Italy [Bologna]), M. Giroletti (INAF Bologna; Bologna), F. Ambrosino (INAF – Osservatorio Astronomico di Roma, Rome, Italy [INAF Roma]); INAF – Istituto Astrofisica Planetologia Spaziali, Rome, Italy; Sapienza Università di Roma, Rome, Italy), S.Crespi (NYU Abu Dhabi), A. Miraval Zanon (Agenzia Spaziale Italiana, Rome, Italy; INAF Roma), X. Hou (Yunnan Observatories, Chinese Academy of Sciences, Kunming, China; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, China), D. Li (National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China; University of Chinese Academy of Sciences, Beijing, China; Research Center for Intelligent Computing Platforms, Zhejiang Laboratory, Hangzhou, China), J. Li (CAS Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China, Hefei, China; School of Astronomy and Space Science, University of Science and Technology of China, Hefei, China), P. Wang (Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing, China), D. M. Russell (NYU Abu Dhabi), D. F. Torres (INAF Brera; IEEC; Institució Catalana de Recercai Estudis Avançats, Barcelona, Spain), K. Alabarta (NYU Abu Dhabi), P. Casella (INAF Roma), S. Covino (INAF Brera), D. M. Bramich (NYU Abu Dhabi; Division of Engineering, New York University Abu Dhabi, UAE), D. de Martino (INAF − Osservatorio Astronomico di Capodimonte, Napoli, Italy), M. Méndez (Kapteyn Astronomical Institute, University of Groningen, Groningen, The Netherlands), S. E. Motta (INAF Brera), A. Papitto (INAF Roma), P. Saikia (NYU Abu Dhabi), and F. Vincentelli (Instituto de Astrofísica de Canarias, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain).
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Contacts
Maria Cristina Baglio
New York University Abu Dhabi and Italian National Institute for Astrophysics (INAF)
Abu Dhabi, United Arab Emirates
Tel: +97126287089
Email: mcb19@nyu.edu ; maria.baglio@inaf.it
Francesco Coti Zelati
Institute of Space Sciences
Barcelona, Spain
Tel: (+34) 937379788 430416
Email: cotizelati@ice.csic.es
Sergio Campana
INAF Brera Observatory
Merate, Italy
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Email: sergio.campana@brera.inaf.it
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