Dust in the interplanetary medium

Mann, Ingrid; Czechowski, A.; Meyer‐Vernet, N.; Zaslavsky, A.; Lamy, H.

doi:10.1088/0741-3335/52/12/124012

Cited by 31 publications

(35 citation statements)

References 24 publications

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“…According to modern data, the den sity of interplanetary dust decreases with increasing distance from the Sun; there is almost no dust at a dis tance of more than 3 AU. About two thirds of inter planetary dust is concentrated in particles with a mass of g ranging in size from one to ten microns (Mann et al, 2010). The total mass of the dust is esti mated approximately as g (Sunyaev, 1986).…”

Section: Anticipated Effects Of the Change In The Sun's Massmentioning

confidence: 99%

Changes in the Sun’s mass and gravitational constant estimated using modern observations of planets and spacecraft

Pitjeva

Pitjev

2012

Sol Syst Res

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More than 635 000 positional observations of planets and spacecraft of different types, mostly radiotechnical ones , have been used for estimating possible changes of the gravitation constant, the solar mass, and semi-major axes of planets, as well as the value of the astronomical unit, related to them. The analysis of the observations has been performed on the basis of the EPM2010 ephemerides of IAA RAS in post-newtonian approximation.The EPM ephemerides are computed by numerical integration of the equations of motion of the nine major planets, the Sun, the Moon, asteroids and trans-neptunian objects.The estimation of change for the geliocentric gravitation constant GM ⊙ has been obtainedThe positive century changes of semi-major axes ȧi /a i have been determined simultaneously for the planets Mercury, Venus, Mars, Jupiter, Saturn provided with high-accuracy sets of the observations, as expected if the geliocentric gravitation constant is decreasing in century wise. Perhaps, loss of the mass of the Sun M ⊙ the produces change of GM ⊙ due to the solar radiation and the solar wind compensated partially by the matter dropping on the Sun.It was been found from the obtained GM ⊙ change and taking into account the maximal limits of the possible M ⊙ change that the gravitation constant Ġ/G falls within the interval −4.2 • 10 −14 < Ġ/G < +7.5 • 10 −14 in year with the 95% probability.The astronomical unit (au) is only connected with the geliocentric gravitation constant by its definition. The decrease of GM ⊙ obtained in this paper should correspond to the century decrease of au. However, it has been shown that the present accuracy level of observations does not permit to evaluate the au change. The attained possibility of fining the GM ⊙ change from high-accuracy observations points that fixing the connection between GM ⊙ and au at the certain time moment is desirable, as it is inconvenient highly to have the changing value of the astronomical unit.

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Section: Anticipated Effects Of the Change In The Sun's Massmentioning

confidence: 99%

Changes in the Sun’s mass and gravitational constant estimated using modern observations of planets and spacecraft

Pitjeva

Pitjev

2012

Sol Syst Res

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“…The dust larger than 10 −15 kg is in Keplerian orbits. Further discussion can be found in the reference Mann et al (2010b). 0.038N p < N α < 0.048N p (Klecker, 2009;Schwenn, 1983) for the alpha particle density, we get 0.15 < S α < 0.19. In the simple model of Eq.…”

Section: An Extended Version Of the Treumann And Baumjohann Modelmentioning

confidence: 58%

“…One can estimate average values of the velocity of nanodust based on trajectory calculations when assuming a model of dust production inside 1 AU. Figure 2 shows such a model based on discussions in Mann et al (2010b) in comparison to the velocities of the larger dust particles. One can see that the nanodust particles with masses m ≤ 10 −19 kg have velocities ∼300 km s −1 ; the dust particles approximately in the mass interval 10 −19 kg ≤ m ≤ 10 −14 kg are significantly influenced by radiation pressure and depending on their optical properties can be repelled from the Sun.…”

Section: Dust Trajectories In the Solar Windmentioning

confidence: 99%

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

Mann

Hamrin

2013

Ann. Geophys.

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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.

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“…The total mass of the dust cloud inside Jupiter's orbit is estimated to be between ∼10 −9 and ∼10 −8 M ⊕ [21,23]. The mass density of interplanetary dust close to the Earth's orbit is roughly comparable to that of the solar wind [24].…”

Section: Basic Factsmentioning

confidence: 98%

Exozodiacal clouds: hot and warm dust around main sequence stars

Kral

Krivov

Defrère

et al. 2017

Astronomical Review

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A warm/hot dust component (at temperature >300 K) has been detected around ∼20% of A, F, G, K stars. This component is called 'exozodiacal dust' as it presents similarities with the zodiacal dust detected in our solar system, even though its physical properties and spatial distribution can be significantly different. Understanding the origin and evolution of this dust is of crucial importance, not only because its presence could hamper future detections of Earthlike planets in their habitable zones, but also because it can provide invaluable information about the inner regions of planetary systems. In this review, we present a detailed overview of the observational techniques used in the detection and characterisation of exozodiacal dust clouds ('exozodis') and the results they have yielded so far, in particular regarding the incidence rate of exozodis as a function of crucial parameters such as stellar type and age, or the presence of an outer cold debris disc. We also present the important constraints that have been obtained, on dust size distribution and spatial location, using state-of-the-art radiation transfer models on some of these systems. Finally, we investigate the crucial issue of how to explain the presence of exozodiacal dust around so many stars (regardless of their ages) despite the fact that such dust so close to its host star should disappear rapidly due to the coupled effect of collisions and stellar radiation forces. Several potential mechanisms have been proposed to solve this paradox and are reviewed in detail in this paper. The review finishes by presenting the future of this growing field.

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Dust in the interplanetary medium

Cited by 31 publications

References 24 publications

Changes in the Sun’s mass and gravitational constant estimated using modern observations of planets and spacecraft

Changes in the Sun’s mass and gravitational constant estimated using modern observations of planets and spacecraft

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

Exozodiacal clouds: hot and warm dust around main sequence stars

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