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In early 2008, German magazine publisher Bauer bought the radio division of British company Emap, which had been established as East Midland Allied Press in 1947.[1] Consequently, Emap Radio Limited was renamed to Bauer Radio Limited.[2]

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In April 2011, Bauer Radio announced it would be restructuring its radio portfolio into two divisions. Stations linked to geographic areas would come under the Bauer Place brand, while national stations such as Kiss, Kerrang and The Hits would come under Bauer Passion. The Big City Network identity was dropped as part of the restructuring.[4]

In September 2014, Bauer announced it would be restructuring its radio portfolio as from January 2015. Magic AM in England was dropped in favour of the stations reverting to their heritage station names.[6][7] The stations then formed part of the new 'City 2' network serving both Scotland and Northern England. A 'City 3' network on DAB, replacing The Hits Radio in most areas, launched on 19 January 2015. As part of this restructuring, the Place and Passion network banners introduced in 2011 were replaced by the Bauer City and Bauer National divisions. The 'City 3' network was withdrawn in favour of reverting to the networked The Hits service from September 2017.

On 6 May 2016, Bauer announced it had bought Midlands radio group Orion Media for an undisclosed amount, reportedly between 40 and 50 million.[9][10] It was subsequently confirmed that Orion's stations Free Radio (West Midlands) and Gem (East Midlands) would become part of the Bauer City portfolio, with Gem introducing a version of the City sonic logo device to its presentation from August 2016.

The Wireless Group and Emap entered into a venture to run the following three DAB multiplexes. These multiplexes were initially branded as TWG-Emap multiplexes; following the sale of TWG to UTV (creating UTV Radio), the multiplexes were relabelled as UTV-Emap, and following the sale of Emap's radio assets to Bauer, the blocks were renamed again as UTV-Bauer. Bauer owned 30 per cent of the UTV-Bauer venture, but sold its stake in November 2013.[21] Now wholly owned by Bauer Radio following the sale of the Wireless local stations in 2019.

In March 2023, Bauer announced that all its radio stations and audio content across Europe would be available in once place, named Rayo.[23] Rayo will be an app and website, replacing its existing radio station apps and Planet Radio website.

With Planet, planning engineers can deliver higher quality radio network designs within the ever-tighter budgets and shorter deadlines demanded by the business. 3D simulation technologies, underpinned by machine learning and multiple live data sources, help you create more accurate designs. While comprehensive what-if scenario planning ensures maximum return on CAPEX investments and automation of planning tasks increases engineering efficiency, reducing the time-to-market of new designs.

The detection of multiple coherent radio bursts from YZ Cet prompts the question of whether the planets in the system could have powered the radio bursts. To answer this question, we must estimate the magnetized environment of YZ Ceti, and calculate the strength of the potential SPI.

For the environment, we adopted an isothermal stellar wind model for the YZ Cet system. The planets have orbital distances of 20 stellar radii or more21 that are unlikely to be encompassed by closed stellar magnetic field lines, and thus the planets are probably intersecting open field lines that carry the stellar wind. We use two fiducial wind models (Methods). Model A assumes an open magnetic field entrained by a strong radial wind launched from the stellar surface, matching assumptions commonly used in approximate calculations in the literature (for example, refs. 7,9). Model B uses a weaker wind and a potential field source surface (PFSS) extrapolation to account for a closed field near the star. Incorporating a closed field region near the stellar surface, in particular, should provide a more realistic estimate of the radial field decay of any magnetized star. Uncertain model assumptions, regarding stellar mass-loss rate and magnetic field strength, can impact whether a planet orbits in the sub- or super-Alfvnic regime. Encouragingly, both of our fiducial models find that the innermost planets are within the sub-Alfvnic regime, allowing the planetary perturbation of the stellar magnetic field to communicate energy back towards the stellar surface to induce gigahertz emission. We expand on the effects of exploring the wind-model parameter space in Methods.

There are many uncertain assumptions that go into these SPI flux predictions, which in effect allow the prediction curves of Fig. 3 to move up and down by several factors. Nevertheless, following our best characterization of the system (model B), our calculations suggest that if the reconnection framework is an accurate description of the physics, then the bursts could readily be produced by YZ Cet b through SPI. Interestingly, if the Alfvn wing scenario is more applicable to these systems, then the radio detections would imply a substantial planetary magnetic field for the terrestrial planet.

After modelling the flux density of the detected radio bursts, we also considered their relative timing to evaluate their potential SPI nature. In Jupiter, the observed recurrence of the Io-induced radio emissions depends on both the orbital period Porb and the rotation period Prot of the tilted Jovian magnetic field (see within ref. 26). These define the synodic period (\({P}_{{{{\rm{syn}}}}}={[{P}_{{{{\rm{orb}}}}}^{-1}-{P}_{{{{\rm{rot}}}}}^{-1}]}^{-1}\)) at which the satellite orbit returns to the same position relative to the host magnetic field. Reference 27 discussed the possible SPI periodicities in depth, noting the importance of the synodic period and half-synodic period, the latter defining a similar satellite position, but on the opposite side of the host magnetic field.

To determine whether SPIs could have powered our observed polarized radio emissions we needed to characterize the likely magnetospheric environment impacting the YZ Cet planetary system. We considered two models: (1) a magnetosphere defined by a radial isothermal stellar wind whose properties are set by the corona and the surface magnetic field strength, and (2) a PFSS extrapolation of typical M-dwarf ZDI measurements including an isothermal stellar wind solution beyond the source surface40. As the magnetic field and wind environments of low-mass stars are very uncertain, this approach explores the effects of a range of likely stellar magnetic field strengths experienced by the YZ Cet planets.

The first approach, often employed in the literature, uses a stellar wind originating from the stellar surface, which overestimates the magnetic field at the planet location because it does not take into account the rapid radial decay of closed field lines near the stellar surface (for example, ref. 7). The second approach accounts for this effect by using a more realistic stellar magnetic field topology (for example, ref. 40); however, the inherent assumptions exclude additional stresses to the magnetic field, and may underestimate the strength of the magnetic field at planetary distances from the star, beyond a poorly constrained source surface.

We further illustrate some properties of model B in Supplementary Fig. 8, showing the velocities relevant to the wind (top panel), and the total wind pressure throughout the model environment around YZ Cet. We considered model B to correspond to our most realistic estimate of the average magnetized environment pervading this planetary system, whereas model A encapsulates typical assumptions in the literature treatment of these questions. While informed by the literature, the wind parameters are typically uncertain for low-mass stars, but as we employed an analytic model, we can readily change the input assumptions to determine their effect on the potential for the YZ Cet planetary system to power radio emissions (see below). To provide some intuition for the isothermal wind solution and the impacts of these parameter assumptions, we note that changing the temperature is the most impactful parameter determining the wind velocity, changes in the mass-loss rate largely impact the wind density, and the radial field strength scales the overall magnetic field as the azimuthal field component is much weaker for slowly rotating systems. In the absence of a three-dimensional wind simulation (for example, ref. 15), these simplified isothermal approaches provide a reasonable means to examine the approximate interplanetary environment conditions53.

Our detection of polarized radio bursts from YZ Cet prompts the question of whether the coherent radio emission could have been powered by the magnetic interaction of the star with its planets (see within ref. 1). We used models A and B (described above), to define the magnetized stellar wind filling the environment of the YZ Cet planetary system. When this wind interacts with the planets, the dissipated energy can power auroral radio emissions. We estimated the available power through this interaction using the frameworks of ref. 25 (reconnection) and ref. 6 (Alfvn wings), similar to the approach taken by ref. 9.

The last remaining variable in the power expressions is the planetary obstacle radius, Ro. This is defined by the size of the planetary magnetosphere, or at a minimum the radius of the planet itself assuming a thin ionosphere. We use the pressure balance between the supposed planetary field and the wind to define the radius of the planetary magnetopause:

With these assumptions, we can compute the energy available to power auroral radio bursts from YZ Cet, using both the reconnection and Alfvn wing prescriptions, as well as considering both the model A and model B wind environments. To convert the power to a possible burst radio flux density we use e24fc04721