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Evidence for radio and X-ray auroral emissions from the magnetic B-type star
{ho} Oph A | P. Leto
; C. Trigilio
; F. Leone
; I. Pillitteri
; C.S. Buemi
; L. Fossati
; F. Cavallaro
; L.M. Oskinova
; R. Ignace
; J. Krticka
; G. Umana
; G. Catanzaro
; A. Ingallinera
; F. Bufano
; C. Agliozzo
; N.M. Phillips
; L. Cerrigone
; S. Riggi
; S. Loru
; M. Munari
; M. Gangi
; M. Giarrusso
; J. Robrade
; | Date: |
21 Feb 2020 | Abstract: | We present new ATCA multi-wavelength radio measurements (range 2.1-21.2 GHz)
of the early-type magnetic star
{ho} Oph A, performed in March 2019 during 3
different observing sessions. These new ATCA observations evidence a clear
rotational modulation of the stellar radio emission and the detection of
coherent auroral radio emission from
{ho} Oph A at 2.1 GHz. We collected
high-resolution optical spectra of
{ho} Oph A acquired by several instruments
over a time span of about ten years. We also report new magnetic field
measurements of
{ho} Oph A that, together with the radio light curves and the
temporal variation of the equivalent width of the HeI line ({lambda}=5015
{AA}), were used to constrain the rotation period and the stellar magnetic
field geometry. The above results have been used to model the stellar radio
emission, modelling that allowed us to constrain the physical condition of
{ho} Oph A’s magnetosphere. Past XMM measurements showed periodic X-ray
pulses from
{ho} Oph A. We correlate the X-ray light curve with the magnetic
field geometry of
{ho} Oph A. The already published XMM data have been
re-analyzed showing that the X-ray spectra of
{ho} Oph A are compatible with
the presence of a non-thermal X-ray component. We discuss a scenario where the
emission phenomena occurring at the extremes of the electromagnetic spectrum,
radio and X-ray, are directly induced by the same plasma process. We interpret
the observed X-ray and radio features of
{ho} Oph A as having an auroral
origin. | Source: | arXiv, 2002.9251 | Services: | Forum | Review | PDF | Favorites |
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