Rotation, spectral variability, magnetic geometry and magnetosphere of the Of?p star CPD -28 2561

TL;DR

This study investigates the magnetic field, spectral variability, and magnetospheric structure of the Of?p star CPD -28 2561, revealing a 73.41-day rotation period and evidence of a co-rotating magnetosphere influencing spectral lines.

Contribution

It provides the first detailed magnetic and spectroscopic analysis of CPD -28 2561, including a magnetic field measurement, period determination, and magnetospheric modeling, advancing understanding of Of?p star magnetospheres.

Findings

Detected a weak sinusoidal magnetic field variation (~565 G to -335 G).

Identified a 73.41-day stellar rotation period.

Modeled a magnetosphere with a dipole field strength of ~2.6 kG.

Abstract

We report magnetic and spectroscopic observations and modeling of the Of?p star CPD -28 2561. Using more than 75 new spectra, we have measured the equivalent width variations and examined the dynamic spectra of photospheric and wind-sensitive spectral lines. A period search results in an unambiguous 73.41 d variability period. High resolution spectropolarimetric data analyzed using Least-Squares Deconvolution yield a Zeeman signature detected in the mean Stokes V profile corresponding to phase 0.5 of the spectral ephemeris. Interpreting the 73.41 d period as the stellar rotational period, we have phased the equivalent widths and inferred longitudinal field measurements. The phased magnetic data exhibit a weak sinusoidal variation, with maximum of about 565 G at phase 0.5, and a minimum of about -335 G at phase 0.0, with extrema approximately in phase with the (double-wave) Halpha equivalent width variation. Modeling of the Halpha equivalent width variation assuming a quasi-3D magnetospheric model produces a unique solution for the ambiguous couplet of inclination and magnetic obliquity angles: (i, beta) or (beta, i)=(35 deg,90 deg). Adopting either geometry, the longitudinal field variation yields a dipole polar intensity Bd=2.6\pm 0.9~kG, consistent with that obtained from direct modelling of the Stokes V profiles. We derive a wind magnetic confinement parameter eta*\simeq 100, leading to an Alfv\'en radius RA\simeq 3-5~R*, and a Kepler radius RK\simeq 20~R*. This supports a physical scenario in which the Halpha emission and other line variability have their origin in an oblique, co-rotating 'dynamical magnetosphere' structure resulting from a magnetically channeled wind. Nevertheless, the details of the formation of spectral lines and their variability within this framework remain generally poorly understood.