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Observations of Strong Magnetic Fields in Nondegenerate Stars

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The Strongest Magnetic Fields in the Universe

Part of the book series: Space Sciences Series of ISSI ((SSSI,volume 54))

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Abstract

We review magnetic-field measurements of nondegenerate stars across the Hertzprung–Russell diagram for main sequence, premain sequence, and postmain sequence stars. For stars with complex magnetic-field morphologies, which includes all G–M main sequence stars, the analysis of spectra obtained in polarized vs unpolarized light provides very different magnetic measurements because of the presence or absence of cancellation by oppositely directed magnetic fields within the instrument’s spatial resolution. This cancellation can be severe, as indicated by the spatially averaged magnetic field of the Sun viewed as a star. These averaged fields are smaller by a factor of 1000 or more compared to spatially resolved magnetic-field strengths. We explain magnetic-field terms that characterize the fields obtained with different measurement techniques. Magnetic fields typically control the structure of stellar atmospheres in and above the photosphere, the heating rates of stellar chromospheres and coronae, mass and angular momentum loss through stellar winds, chemical peculiarity, and the emission of high energy photons, which is critically important for the evolution of protoplanetary disks and the habitability of exoplanets. Since these effects are governed by the star’s magnetic energy, which is proportional to the magnetic-field strength squared and its fractional surface coverage, it is important to measure or reliably infer the true magnetic-field strength and filling factor across a stellar disk. We summarize magnetic-field measurements obtained with the different observing techniques for different types of stars and estimate the highest magnetic-field strengths. We also comment on the different field morphologies observed for stars across the H–R diagram, typically inferred from Zeeman-Doppler imaging and rotational modulation observations.

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Abbreviations

BBLP:

Broad-band linear polarization

BOB:

B fields in OB stars consortium

CFHT:

Canada-France-Hawaii Telescope

CP:

Chemically preculiar A- and B-type stars

CRIRES:

CRyogenic high-resolution InfraRed Echelle Spectrograph

DI:

Doppler imaging

ESO:

European Southern Observatory

\(\mathrm{ESP}_{a}\mathrm{DO}_{n}\mathrm{S}\) :

a high-resolution spectrograph on the CFHT telescope

FEROS:

Fiber-fed Extended Range Optical Spectrograph

FORS1:

FOcal Reducer and low dispersion Spectrograph

FORS2:

New version of FORS1

FUV:

Far ultraviolet (912–1700 Å)

GTO:

Guaranteed time observer

HARPS:

High Accuracy Radial Velocity Planet Searcher

HARPSpol:

HARPS with polarizing optics

HINODE:

Solar-B satellite

IVQU:

Components of the Stokes polarimetry vector

LTE:

Local thermodynamic equilibrium

LSD:

Least-squares deconvolution

MDI:

Michelson Doppler imager

MHD:

Magnetohydrodynamics

MiMeS:

Magnetism in Massive Stars collaboration

MOST:

Microvariability and Oscillations of STars satellite

NIM:

Near Infrared Magnetograph

NSO:

National Solar Observatory

RGB:

Red giant branch stars

SB:

Spectroscopic binary stars

SOFIN:

An optical high-resolution spectrograph on the Nordic Optical Telescope

SOHO:

Solar and Heliospheric Observatory

SOT:

Solar Optical Telescope

SOT/SP:

SOT Spectropolarimeter

SPB:

Slowly pulsating B-type stars

SVD:

Singular value decomposition method for Stokes profile reconstruction

UV:

Ultraviolet (912–3000 Å)

VLT:

Very Large Telescope

ZAMS:

Zero-age main sequence

ZDI:

Zeeman Doppler imaging

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Authors and Affiliations

  1. JILA/University of Colorado and NIST, Boulder, CO, USA

    Jeffrey L. Linsky

  2. European Southern Observatory, Garching, Germany

    Markus Schöller

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  1. Jeffrey L. Linsky
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  2. Markus Schöller
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Correspondence to Jeffrey L. Linsky .

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Editors and Affiliations

  1. Russian Academy of Sciences, Moscow, Russia

    V.S. Beskin

  2. The Blackett Laboratory, Imperial College London, London, United Kingdom

    A. Balogh

  3. International Space Science Institute, Bern, Switzerland

    M. Falanga

  4. Purdue University, West Lafayette, Indiana, USA

    M. Lyutikov

  5. INAF-IASF Milano, Milano, Italy

    S. Mereghetti

  6. The Hebrew University, Racah Institute for Physics, Jerusalem, Israel

    T. Piran

  7. International Space Science Institu, Bern, Switzerland

    R.A. Treumann

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Linsky, J.L., Schöller, M. (2016). Observations of Strong Magnetic Fields in Nondegenerate Stars. In: Beskin, V., et al. The Strongest Magnetic Fields in the Universe. Space Sciences Series of ISSI, vol 54. Springer, New York, NY. https://doi.org/10.1007/978-1-4939-3550-5_3

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