Details

Autor(en) / Beteiligte

• Marino, A
• Malzac, J
• Del Santo, M
• Migliari, S
• Belmont, R
• Di Salvo, T
• Russell, D M
• Lopez Miralles, J
• Perucho, M
• D’Aì, A
• Iaria, R
• Burderi, L

Titel

Testing jet geometries and disc–jet coupling in the neutron star LMXB 4U 0614 + 091 with the internal shocks model

Ist Teil von

• Monthly notices of the Royal Astronomical Society, 2020-11, Vol.498 (3), p.3351-3367

Ort / Verlag

Oxford University Press

Erscheinungsjahr

2020

Quelle

EZB-FREE-00999 freely available EZB journals

Beschreibungen/Notizen

• ABSTRACT Multiwavelength spectral energy distributions of low-mass X-ray binaries (LMXBs) in the hard state are determined by the emission from a jet, for frequencies up to mid-infrared, and emission from the accretion flow in the optical to X-ray range. In the last years, the flat radio-to-mid-IR spectra of black hole (BH) X-ray binaries was described using the internal shocks model, which assumes that the fluctuations in the velocity of the ejecta along the jet are driven by the fluctuations in the accretion flow, described by the X-ray power density spectrum (PDS). In this work, we attempt to apply this model for the first time to a neutron star (NS) LMXB, i.e. 4U 0614 + 091. We used the multiwavelength data set obtained in 2006, comprising data from radio to X-ray, and applied a model that includes an irradiated disc model for the accretion flow and an updated version of the internal shocks code for the ejection. The new version of the code allows to change the geometry of the jet for the case of non-conical jets. Only two alternative scenarios provide a satisfactory description of the data: using the X-ray PDS but in a non-conical geometry for the jet, or either using a conical geometry but with a ‘flicker-noise’ PDS. Both scenarios would imply some differences with the results obtained with similar models on BH X-ray binaries, shedding light on the possibility that jets in NS and BH binaries might somehow have a different geometry or a different coupling with the accretion flow.