Candidate 1.97 keV absorption line in HLX 2SXPS J111416.1+481833 interpreted as proton CRSF implying B ~ 4e14 G for a neutron star accretor.
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X-ray timing and spectral analysis of ASKAP J174508.9-505149 detects matching periodicity and features consistent with an accreting magnetic CV.
Pulsational mass loss from supermassive stars ejects discrete shells that form the compact dense gas cocoons observed in Little Red Dots.
Simulations show VMS in star clusters reach 10^3-10^4 solar masses with dimensionless spins >10 under bloated accretion conditions, potentially forming spinning IMBHs that produce GW bursts like GW190521.
citing papers explorer
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Discovery of a Candidate 2 keV Cyclotron Resonance Scattering Feature in the HLX NGC 3583 X-1
Candidate 1.97 keV absorption line in HLX 2SXPS J111416.1+481833 interpreted as proton CRSF implying B ~ 4e14 G for a neutron star accretor.
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The X-ray emission of the long-period transient and accreting cataclysmic variable ASKAP J174508.9-505149
X-ray timing and spectral analysis of ASKAP J174508.9-505149 detects matching periodicity and features consistent with an accreting magnetic CV.
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Pulsational mass loss from supermassive stars creates the compact shells of Little Red Dots
Pulsational mass loss from supermassive stars ejects discrete shells that form the compact dense gas cocoons observed in Little Red Dots.
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Mass and Spin Growth of Very Massive Stars in Star Clusters Potentially Associated with Little Red Dots
Simulations show VMS in star clusters reach 10^3-10^4 solar masses with dimensionless spins >10 under bloated accretion conditions, potentially forming spinning IMBHs that produce GW bursts like GW190521.