Stellar magnetic cycles

Lanza, A. F.

doi:10.1017/s1743921309992523

Cited by 13 publications

(7 citation statements)

References 64 publications

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“…For magnetically active stars developing starspots at their surface, the global brightness is modulated as a function of the position and the size of the spots over the visible stellar disk with a period that is related to the rotation period of the star at the active latitude where the spot appears (e.g. Lanza 2010;Fröhlich et al 2012;Lanza et al 2014;McQuillan et al 2014). As the magnetic cycle evolves, the number and size of the spots change.…”

Section: From the Direct Analysis Of The Light Curvesmentioning

confidence: 99%

Asteroseismology of solar-type stars

García

Ballot

2019

Living Rev Sol Phys

154

100

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Until the last few decades, investigations of stellar interiors had been restricted to theoretical studies only constrained by observations of their global properties and external characteristics. However, in the last 30 years the field has been revolutionized by the ability to perform seismic investigations of stellar interiors. This revolution begun with the Sun, where helioseismology has been yielding information competing with what can be inferred about the Earth’s interior from geoseismology. The last two decades have witnessed the advent of asteroseismology of solar-like stars, thanks to a dramatic development of new observing facilities providing the first reliable results on the interiors of distant stars. The coming years will see a huge development in this field. In this review we focus on solar-type stars, i.e., cool main-sequence stars where oscillations are stochastically excited by surface convection. After a short introduction and a historical overview of the discipline, we review the observational techniques generally used, and we describe the theory behind stellar oscillations in cool main-sequence stars. We continue with a complete description of the normal mode analyses through which it is possible to extract the physical information about the structure and dynamics of the stars. We then summarize the lessons that we have learned and discuss unsolved issues and questions that are still unanswered.

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Section: From the Direct Analysis Of The Light Curvesmentioning

confidence: 99%

Asteroseismology of solar-type stars

García

Ballot

2019

Living Rev Sol Phys

154

100

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“…The reliance of society on space-based technology has reached a point where understanding the origin, evolution, and multifaceted impacts of the Sun's magnetism has reached a heightened level of importance in astrophysics. Beyond this very practical issue, there is an implicit understanding that unlocking the puzzle around the origins of the Sun's magnetism could provide vital clues to the origins and behavior of the magnetic field in other stars (see, e.g., Lanza, 2010).…”

Section: Abstract: Sun: Magnetism Sun: Interior Sun: Rotation Solamentioning

confidence: 99%

The Extended Solar Cycle: Muddying the Waters of Solar/Stellar Dynamo Modeling or Providing Crucial Observational Constraints?

Srivastava

McIntosh

Arge

et al. 2018

Front. Astron. Space Sci.

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In 1844 Schwabe discovered that the number of sunspots increased and decreased over a period of about 11 years, that variation became known as the sunspot cycle. Almost eighty years later, Hale described the nature of the Sun's magnetic field, identifying that it takes about 22 years for the Sun's magnetic polarity to cycle. It was also identified that the latitudinal distribution of sunspots resembles the wings of a butterfly showing migration of sunspots in each hemisphere that abruptly start at mid-latitudes towards the Sun's equator over the next 11 years. These sunspot patterns were shown to be asymmetric across the equator. In intervening years, it was deduced that the Sun (and sun-like stars) possess magnetic activity cycles that are assumed to be the physical manifestation of a dynamo process that results from complex circulatory transport processes in the star's interior. Understanding the Sun's magnetism, its origin and its variation, has become a fundamental scientific objective -the distribution of

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“…There is some evidence that cycle periods for solar-type stars with moderate rotation rates tend to decrease somewhat with U but there is much scatter and there may be multiple branches signifying distinct dynamo regimes. We refer the interested reader to the reviews by Rempel [47], Saar [42] and Lanza [48]. Still, it is clear that the interplay between convection and rotation lies at the root of solar and stellar magnetic activity, so we turn now to discuss the nature of convective dynamos.…”

Section: (C) Convection Rotation and Magnetic Activitymentioning

confidence: 99%

The solar dynamo

Miesch

2012

Phil. Trans. R. Soc. A.

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The origins of solar magnetism lie below the visible surface of the Sun, in the highly turbulent convection zone. Turbulent convection operates in conjunction with rotational shear, global circulations and intricate boundary layers to produce the rich diversity of magnetic activity we observe. Here, we review recent insights into the operation of the solar dynamo obtained from solar and stellar observations and numerical models.

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Stellar magnetic cycles

Cited by 13 publications

References 64 publications

Asteroseismology of solar-type stars

Asteroseismology of solar-type stars

The Extended Solar Cycle: Muddying the Waters of Solar/Stellar Dynamo Modeling or Providing Crucial Observational Constraints?

The solar dynamo

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