Formation and Acceleration of Nano Dust in the Inner Heliosphere

Czechowski, A.; Mann, Ingrid

doi:10.1088/0004-637x/714/1/89

Cited by 75 publications

(144 citation statements)

References 30 publications

Supporting

Mentioning

133

Contrasting

Order By: Relevance

“…In the solar system, nanometer-sized particles are detected with the STEREO and Ulysse spacecrafts (Meyer-Vernet et al 2009;Krüger et al 2010, respectively), with an increase in the particle flux in the inner solar system. These very small grains, which are affected by the Lorentz force (Czechowski & Mann 2010), could thus be expected in exozodiacal disks. In fact, magnetic trapping of nanograins could be a valuable alternative to the gas-braking mechanisms we have investigated in this study as discussed by Su et al (2013).…”

Section: Discussionmentioning

confidence: 89%

An interferometric study of the Fomalhaut inner debris disk

Lebreton

Lieshout

Augereau

et al. 2013

A&A

111

View full text Add to dashboard Cite

Context. Debris disks are thought to be extrasolar analogs to the solar system planetesimal belts. The star Fomalhaut harbors a cold debris belt at 140 AU comparable to the Edgeworth-Kuiper belt, as well as evidence of a warm dust component, unresolved by singledish telescopes, which is suspected of being a bright analog to the solar system's zodiacal dust. Aims. Interferometric observations obtained with the VLTI/VINCI instrument and the Keck Interferometer Nuller have identified nearand mid-infrared excesses attributed respectively to hot and warm exozodiacal dust residing in the inner few AU of the Fomalhaut environment. We aim to characterize the properties of this double inner dust belt and to unveil its origin. Methods. We performed parametric modeling of the exozodiacal disk ("exozodi") using the GRaTeR radiative transfer code to reproduce the interferometric data, complemented by mid-to far-infrared photometric measurements from Spitzer and Herschel . A detailed treatment of sublimation temperatures was introduced to explore the hot population at the size-dependent sublimation rim. We then used an analytical approach to successively testing several source mechanisms for the dust and suspected parent bodies. Results. A good fit to the multiwavelength data is found by two distinct dust populations: (1) a population of very small (0.01 to 0.5 μm), hence unbound, hot dust grains confined in a narrow region (∼0.1-0.3 AU) at the sublimation rim of carbonaceous material; (2) a population of bound grains at ∼2 AU that is protected from sublimation and has a higher mass despite its fainter flux level. We propose that the hot dust is produced by the release of small carbon grains following the disruption of dust aggregates that originate in the warm component. A mechanism, such as gas braking, is required to further confine the small grains for a long enough time. In situ dust production could hardly be ensured for the age of the star, so we conclude that the observed amount of dust is triggered by intense dynamical activity. Conclusions. Fomalhaut may be representative of exozodis that are currently being surveyed at near and mid-infrared wavelengths worldwide. We propose a framework for reconciling the "hot exozodi phenomenon" with theoretical constraints: the hot component of Fomalhaut is likely the "tip of the iceberg" since it could originate in the more massive, but fainter, warm dust component residing near the ice line. This inner disk exhibits interesting morphology and can be considered a prime target for future exoplanet research.

show abstract

Section: Discussionmentioning

confidence: 89%

An interferometric study of the Fomalhaut inner debris disk

Lebreton

Lieshout

Augereau

et al. 2013

A&A

111

View full text Add to dashboard Cite

show abstract

“…Qualitative picture of dust trajectories Although the reported calculations didn't use the guiding centre approximation, it helps to understand the nanodust dynamics qualitatively for both trapped and ejected particles ( [6], see Fig. 4).…”

Section: Dust Trajectory Calculationsmentioning

confidence: 99%

“…−5 e/m p that is released from a circular orbit of radius 0.2 AU close to the solar equator plane (shown projected onto this plane [6]). …”

Section: Dust Trajectory Calculationsmentioning

confidence: 99%

See 1 more Smart Citation

Dust in the interplanetary medium

Mann

Czechowski

Meyer‐Vernet

et al. 2010

Plasma Phys. Control. Fusion

View full text Add to dashboard Cite

Abstract. The mass density of dust particles that form from asteroids and comets in the interplanetary medium of the solar system is, near 1AU, comparable to the mass density of the solar wind. It is mainly contained in particles of micrometer size and larger. Dust and larger objects are destroyed by collisions and sublimation and hence feed heavy ions into the solar wind and the solar corona. Small dust particles are present in large number and as a result of their large charge to mass ratio deflected by electromagnetic forces in the solar wind. For nano dust particles of sizes ≃ 1 − 10 nm, recent calculations show trapping near the Sun and outside from about 0.15 AU ejection with velocities close to solar wind velocity. The fluxes of ejected nano dust are detected near 1AU with the plasma wave instrument onboard the STEREO spacecraft. Though such electric signals have been observed during dust impacts before, the interpretation depends on several different parameters and data analysis is still in progress.PACS numbers: 96.30.Vb, 96.50.Ci, 96.50.Dj, 96.50.Ya

show abstract

“…These values of Q/m do not occur for dust in the solar system (see e.g. Czechowski and Mann, 2010), but rather apply to heavy ions. In this context we point out that the influence of the gyration radius has been mentioned before in a different context.…”

Section: Dust Pickup and Fluid Approachmentioning

confidence: 90%

Dust dynamic pressure and magnetopause displacement: reasons for non-detection

Mann

Hamrin

2013

Ann. Geophys.

Self Cite

View full text Add to dashboard Cite

Abstract. In a recent paper, Treumann and Baumjohann (2011) propose that the contribution of dust particles to the solar wind dynamic pressure can cause large compressions of the Earth's magnetopause and suggest that this occurs when Earth encounters meteoroid streams. In this paper we estimate the contribution from charged dust particles to the solar wind dynamical pressure, and we exclude that the dust associated to meteoroid streams can influence the extension of the magnetopause according to the proposed model. A sufficient coupling to the solar wind is only expected for so-called nanodust. However, the dynamic pressure of the nanodust is orders of magnitudes below that of the solar wind, making it unlikely that its variation can be observed in displacements of the magnetopause. We also discuss the equation that the authors use for estimating the extension of the Earth's magnetopause, and conclude that this is not applicable due to the large gyroradius of the nanodust. We finally note that an influence of dust on the extension of a magnetosphere might be quite possible in other astrophysical systems and based on other processes.

show abstract

Formation and Acceleration of Nano Dust in the Inner Heliosphere

Cited by 75 publications

References 30 publications

An interferometric study of the Fomalhaut inner debris disk

An interferometric study of the Fomalhaut inner debris disk

Dust in the interplanetary medium

Dust dynamic pressure and magnetopause displacement: reasons for non-detection

Contact Info

Product

Resources

About