Spectra of the western eROSITA bubbles reveal two uniform components at 0.60 keV and 0.21 keV with sub-solar abundances, plus a geometrical model constraining horizontal size to ~6 kpc but leaving vertical extent uncertain.
Identifying the coronal content with HamStar
2 Pith papers cite this work. Polarity classification is still indexing.
2
Pith papers citing it
years
2026 2verdicts
UNVERDICTED 2representative citing papers
No bursty planet-induced radio emission detected from five inactive M dwarfs; upper limits constrain GJ 367 b magnetosphere to <0.8 G under assumed stellar wind conditions.
citing papers explorer
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The SRG/eROSITA diffuse soft X-ray background II. spectra and morphology of the eROSITA bubbles in the western Galactic hemisphere
Spectra of the western eROSITA bubbles reveal two uniform components at 0.60 keV and 0.21 keV with sub-solar abundances, plus a geometrical model constraining horizontal size to ~6 kpc but leaving vertical extent uncertain.
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Upper Limits on Planet-Induced GHz Radio Emission from Inactive M Dwarfs
No bursty planet-induced radio emission detected from five inactive M dwarfs; upper limits constrain GJ 367 b magnetosphere to <0.8 G under assumed stellar wind conditions.