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    Double Helix Nebula - Wikipedia

    A magnetic torsional wave near the Galactic Centre tr…

    The magnetic field in the central few hundred parsecs of the Milky Way has a dipolar geometry and is substantially stronger than elsewhere in the Galaxy, with estimates ranging up to a milligauss (refs 1–6). Characterization of the magnetic field at the Galactic Centre is important because it can affect the orbits of molecular clouds by exerting a drag on them, inhibit star formation, and could guide a wind of hot gas or cosmic rays away from the central region. …

    The magnetic field in the central few hundred parsecs of the Milky Way has a dipolar geometry and is substantially stronger than elsewhere in the Galaxy, with estimates ranging up to a milligauss (refs 1–6). Characterization of the magnetic field at the Galactic Centre is important because it can affect the orbits of molecular clouds by exerting a drag on them, inhibit star formation, and could guide a wind of hot gas or cosmic rays away from the central region. Here we report observations of an infrared nebula having the morphology of an intertwined double helix about 100 parsecs from the Galaxy's dynamical centre, with its axis oriented perpendicular to the Galactic plane. The observed segment is about 25 parsecs in length, and contains about 1.25 full turns of each of the two continuous, helically wound strands. We interpret this feature as a torsional Alfvén wave propagating vertically away from the Galactic disk, driven by rotation of the magnetized circumnuclear gas disk. The direct connection between the circumnuclear disk and the double helix is ambiguous, but the images show a possible meandering channel that warrants further investigation.

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    Nature

    The new image was obtained using the Multiband Imaging Photometer (MIPS) camera7 on the Spitzer Space Telescope at a wavelength of 24 µm. It reveals the elongated, double helix nebula (DHN) shown in Fig. 1. This nebula clearly extends beyond the edge of the observed field. The full extent of the DHN is evident in mid-infrared images previously obtained with the Midcourse Space Experiment (MSX) satellite (Fig. 10 of ref. 8; see also ref. 26). In the MSX data (Fig. 2), it is possible with hindsight to recognize the double helix, although the sensitivity and spatial resolution are not sufficient to have revealed this structure before the Spitzer observation. The MSX images show that the structure extends towards smaller Galactic latitude (b) from the region observed with Spitzer; it is at least 20 arcmin (50 pc) in length, extending between Galactic longitude l = 0.08, b = 0.5 and l = 0.02, b = 0.80, and it is possibly part of a larger structure (see below). However, there is no evidence in the MSX data that the helical strands persist outside the region observed with MIPS. It is also noteworthy that there is no sign in MSX images of a negative-latitude counterpart to the DHN.

    The spatial resolution is 6 arcsec. At the 8 kpc distance of the Galactic Centre, 1 arcmin corresponds to 2.5 pc. The full region observed extends well to the lower right of the region shown, and consists of a long strip centred on the bright infr…

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    M.M. is grateful to S. Cowley and S. Stolovy for discussions. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Partial support for this work was provided by NASA through an award issued by JPL/Caltech. This re...

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    Authors and Affiliations

    Department of Physics and Astronomy, University of California, California, 90095-1547, Los Angeles, USA Mark Morris & Tuan Do Center for Radiophysics and Space Research, Cornell University, Space Sciences Building, New York, 14853-6801, Ithaca, USA Keven Uchida Authors Mark Morris View author publications You can also search for this author in PubMed Google Scholar Keven Uchida View author publications You can also search for this author in PubMed Google Scholar Tuan Do View author publications You can also search for this author in PubMed Google Scholar

    Corresponding author

    Correspondence to Mark Morris.

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    Competing interests

    Reprints and permissions information is available at npg.nature.com/reprintsandpermissions. The authors declare no competing financial interests.

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