Astrophysics in 2002

Trimble, Virginia; Aschwanden, Markus J.

doi:10.1086/374651

Cited by 9 publications

(4 citation statements)

References 1,723 publications

(1,669 reference statements)

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“…In 2002, the anomalous-viscosity model [6] was presented by Li and Zhang. This model was closer to the real accretion disk [7,8] than other models.…”

Section: Introductionsupporting

confidence: 49%

The radial–azimuthal instability of accretion disk with anomalous viscosity

Chen¹,

Jiang

2014

Can. J. Phys.

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The stability of the accretion disk is solved by numerical simulations when the radial and azimuthal perturbations are considered, where we adopt the anomalous viscosity model, which is close to real accretion disks. The results are discussed in the inner, intermediate, and outer regions of the accretion disk, respectively. With the increase of viscosity, ␣, the thermal mode and the viscous mode, as well as the acoustic modes, become more unstable in the disk dominated by radiation pressure (inner region). The instability is also influenced by the azimuthal perturbation wavenumber, n. With the increase of n, the thermal mode becomes more unstable, while the in-mode and out-mode become more stable no matter if the disk is dominated by radiation pressure or by gas pressure (intermediate and outer regions). There are many differences between our results and others' results, especially in the inner region of the disk, when the anomalous viscosity is considered. PACS Nos.: 97.10.Gz, 94.30.Gm, 66.20.+d, 52.35.Ra.Résumé : Nous solutionnons par simulation numérique le problème de stabilité du disque d'accrétion en tenant compte des perturbations radiales et azimutales, tout en adoptant un modèle anomal de viscosité qui est proche des vrais disques d'accrétion. Avec l'augmentation de la viscosité ␣, les modes thermique et visqueux, aussi bien que les modes acoustiques, deviennent plus instables dans le disque dominé par la pression de radiation (région interne). L'instabilité est aussi influencée par le nombre d'onde n de la perturbation azimutale. Sous l'augmentation de n, le mode thermique devient plus instable, alors que les modes in et out deviennent plus stables dans un disque dominé par la pression de radiation ou du gaz (région intermédiaire et région externe). Il y a plusieurs différences entre nos résultats et ceux d'autres auteurs, spécialement dans la région interne du disque où on envisage la viscosité anomale. [Traduit par la Rédaction]

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“…In 2002, the anomalous-viscosity model [6] was presented by Li and Zhang. This model was closer to the real accretion disk [7,8] than other models.…”

Section: Introductionsupporting

confidence: 49%

The radial–azimuthal instability of accretion disk with anomalous viscosity

Chen¹,

Jiang

2014

Can. J. Phys.

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“…This result on Altair quickly set the stage for further investigations of the phenomenon, with a variety of instruments and technique coming to bear on this particular object, along with other additional rapid rotators, beginning with Achernar the following year (as will be discussed in the next section, §5.2). This result was noted in the general astrophysical review literature as being a significant development (Trimble & Aschwanden 2003). With Altair, Ohishi et al (2004) followed the initial result with observations of the star with the Navy Optical Interferometer (NOI).…”

Section: Altairmentioning

confidence: 82%

Interferometric observations of rapidly rotating stars

Belle

2012

Astron Astrophys Rev

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Optical interferometry provides us with a unique opportunity to improve our understanding of stellar structure and evolution. Through direct observation of rotationally distorted photospheres at sub-milliarcsecond scales, we are now able to characterize latitude dependencies of stellar radius, temperature structure, and even energy transport. These detailed new views of stars are leading to revised thinking in a broad array of associated topics, such as spectroscopy, stellar evolution, and exoplanet detection. As newly advanced techniques and instrumentation mature, this topic in astronomy is poised to greatly expand in depth and influence.

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“…where d ∼ 2 kpc is the distance to the Crab Pulsar (71). Given that a large number of plasmoids would merge near the light cylinder of the Crab Pulsar due to tearing instability (26), multiple nanoshots may form a single GRP (e.g., ( 72)).…”

Section: Spectral Analysis For the Mp-grp-associated X-raysmentioning

confidence: 99%

Enhanced x-ray emission coinciding with giant radio pulses from the Crab Pulsar

Enoto

Terasawa

Kisaka

et al. 2021

Science

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Giant radio pulses (GRPs) are sporadic bursts emitted by some pulsars that last a few microseconds and are hundreds to thousands of times brighter than regular pulses from these sources. The only GRP-associated emission outside of radio wavelengths is from the Crab Pulsar, where optical emission is enhanced by a few percentage points during GRPs. We observed the Crab Pulsar simultaneously at x-ray and radio wavelengths, finding enhancement of the x-ray emission by 3.8 ± 0.7% (a 5.4σ detection) coinciding with GRPs. This implies that the total emitted energy from GRPs is tens to hundreds of times higher than previously known. We discuss the implications for the pulsar emission mechanism and extragalactic fast radio bursts.

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Astrophysics in 2002

Cited by 9 publications

References 1,723 publications

The radial–azimuthal instability of accretion disk with anomalous viscosity

The radial–azimuthal instability of accretion disk with anomalous viscosity

Interferometric observations of rapidly rotating stars

Enhanced x-ray emission coinciding with giant radio pulses from the Crab Pulsar

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