Astronomers investigate pulsar PSR J1930+1852 and its pulsar wind nebula
X -ray images of G54.1 + 0.3. Solid circles (dotted) indicate the Source Source (background) regions for Nustar and Xmm-Newton observations. Credit: The astrophysical newspaper (2025). DOI: 10.3847 / 1538-4357 / Add92e
Using satellites Nustar and Xmm-Newton, astronomers from New York University (NYU) Abu Dhabi observed a pulsar known as PSR J1930 + 1852 and its Pulsar wind (PWN). Results of the observation campaign, published in The astrophysical newspaperGive more information on the PWN and the pulsar that feeds it.
Pulsar wind nebulae (Pwne) are structures powered by the wind of energy pulsars. In general, a pulsar wind is made up of loaded particles, and when it collides with the pulsar environment – in particular with the supernova eject slowly – it develops a nebula. Observations show that some Pwnes can produce extended X -ray structures in the form of tails and prominent jets.
G54.1 + 0.3 is a PWN powered by the pulsar PSR J1930 + 1852, which has a great rotation power, a young characteristic age and a spin period of around 137 milliseconds. Previous observations have shown that G54.1 + 0.3 is among the several Pwnes which lack an obvious shell associated with a resident supernova shock (SNR).
A team of astronomers led by Jason Alford de Nyu Abu Dhabi recently decided to take a closer look at PSR J1930 + 1852 and its associated PWN.
“In this article, we present a complete analysis of the spectrum of the X-ray X-ray of the pulsar PSR J1930 + 1852 and its PWN G54.1 + 0.3 with these observations XMM-Newton and Nustar”, wrote the researchers in the article.
Observations detected X -ray emission from the combined pulsar and PWN system up to around 70 KEV. The emission of G54.1 + 0.3 itself was detected up to around 30 KEV, with an index of photons from around 1.9 to 2.4 and with photon energy in the range of 3 to 30 Kev.
By analyzing the X -ray spectrum of G54.1 + 0.3, astronomers have noted that it is consistent with a broken power law, with a rupture energy at a level of 5 kev. The energy of the maximum particles for this PWN has been calculated at 400 TEV.
In addition, the study revealed that G54.1 + 0.3 has an age characteristic of 2,830 years and that its magnetic field was estimated at around 7 µg. The spin period of the pulsar PSR J1930 + 1852 was forced to approximately 137.2 milliseconds.
Astronomers compared the properties of G54.1 + 0.3 and PSR J1930 + 1852 to other pulsars with a young Pwne (with characteristic ages of less than 5,000 years). They found that the pulsar studied and its nebula have typical parameters among this group. However, G54.1 + 0.3 is not particularly powerful for its age.
Summarizing the results, astronomers noted that other studies on PSR J1930 + 1852 and its PWNs are necessary in order to better limit parameters such as the braking index, the rotation time scale and the initial pulsar rotation period.
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More information:
Jaj Alford et al, Nustar and Xmm-Newton Observations of the PSR J1930 + 1852 and its nebula of the Pulsar wind, The astrophysical newspaper (2025). DOI: 10.3847 / 1538-4357 / Add92e
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