Adventures in Cosmogony

Cameron, A. G. W.

doi:10.1146/annurev.astro.37.1.1

Cited by 4 publications

(5 citation statements)

References 54 publications

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“…The concept of Babcock was further developed byLeighton (13), who introduced the notion of surface flux transport for the buildup of the polar fields in connection with the dynamo process. More recently, surface flux transport models successfully reproduced the observed evolution of the surface fields and, in particular, the polar fields on the basis of the observed records of sunspot groups as flux input(14)(15)(16)(17)(18). This implies that the tilt of the larger bipolar magnetic regions determines the polar fields.…”

mentioning

confidence: 94%

The crucial role of surface magnetic fields for the solar dynamo

Cameron

Schüßler

2015

Science

145

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The basic concept for the large-scale solar dynamo involves a cycle during which the poloidal field and the toroidal field are mutually generated by one another (1, 2). The winding of the poloidal field by differential rotation creates a toroidal field. A reversed poloidal field results from the formation of magnetic loops in the toroidal field, which become twisted by the Coriolis force due to solar rotation. In turn, the reversed poloidal field then becomes the source of a reversed toroidal field. In this way, the 11-year cycle of solar activity is connected to a 22-yr 1

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mentioning

confidence: 94%

The crucial role of surface magnetic fields for the solar dynamo

Cameron

Schüßler

2015

Science

145

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“…Magnetospheric accretion models, such as those proposed in [37,140,188], provide magnetic links between the star and regions of the disc beyond R co which are rotating more slowly than the star. By having field lines threading the disc at a range of radii the star is able to accrete material without experiencing a net spin-up torque, which would act to slowly increase the stellar rotation rate.…”

Section: Magnetospheric Accretion Models With Dipolar Magnetic Fieldsmentioning

confidence: 99%

The magnetic fields of forming solar-like stars

Gregory¹,

Jardine²,

Gray³

et al. 2010

Rep. Prog. Phys.

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Magnetic fields play a crucial role at all stages of the formation of low-mass stars and planetary systems. In the final stages, in particular, they control the kinematics of in-falling gas from circumstellar discs, and the launching and collimation of spectacular outflows. The magnetic coupling with the disc is thought to influence the rotational evolution of the star, while magnetized stellar winds control the braking of more evolved stars and may influence the migration of planets. Magnetic reconnection events trigger energetic flares which irradiate circumstellar discs with high energy particles that influence the disc chemistry and set the initial conditions for planet formation. However, it is only in the past few years that the current generation of optical spectropolarimeters has allowed the magnetic fields of forming solar-like stars to be probed in unprecedented detail. In order to do justice to the recent extensive observational programs new theoretical models are being developed that incorporate magnetic fields with an observed degree of complexity. In this review we draw together disparate results from the classical electromagnetism, molecular physics/chemistry and the geophysics literature, and demonstrate how they can be adapted to construct models of the large scale magnetospheres of stars and planets. We conclude by examining how the incorporation of multipolar magnetic fields into new theoretical models will drive future progress in the field through the elucidation of several observational conundrums.(Some figures in this article are in colour only in the electronic version) 3.4. Difference between a spherical and Cartesian tensor approach 13 4. Magnetospheric accretion models with multipolar magnetic fields 14 4.1. Development of PFSS models and comparison with MHD field extrapolations 14 4.2. Potential field models of T Tauri magnetospheres with complex fields 16 4.3. 3D MHD models of T Tauri magnetospheres with non-dipolar fields 18 5. Summary and applications to outstanding problems 19 Acknowledgments 21 Appendix A. Relations between the equatorial and polar field strength for a multipole of arbitrary order l 21 Appendix A.1. Odd-order multipoles 21 Appendix A.2. Even-order multipoles 22 Appendix B. Electrostatic expansion using Cartesian tensors 22 Appendix B.1. The dipole term 23 Appendix B.2. The quadrupole term 23 References 24

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“…The four have told their own versions of the story (Hoyle 1982, Fowler 1992, E.M. Burbidge 1994, G.R. Burbidge 2007, as have Cameron (1999), Salpeter (2002), Bethe (2003), and Opik (1977), the last addressing many of his innovative ideas in astrophysics but not the triple alpha reaction.…”

Section: Synthesis In Stars -On Beyond Heliummentioning

confidence: 99%

“…It is perhaps worth reiterating that a chain of neutron captures with intervening beta decays already appears in the work of Walke (1934) who notes that he cannot make Se 74 that way (it is a p-product). Cameron (1999) has provided a particularly clear description of how he was able to estimate the necessary neutron capture cross sections adequately, despite limited laboratory data and very limited computing power at Chalk River. Initially at least his synthesis was less widely known than B 2 FH because the extended version was classified as a Chalk River report (Cameron 1957a) and the public version (Cameron 1957b) was very short.…”

Section: Synthesis In Stars -On Beyond Heliummentioning

confidence: 99%