The Surface Density Distribution in the Solar Nebula

2005 ◽  
Vol 627 (2) ◽  
pp. L153-L155 ◽  
Author(s):  
Sanford S. Davis
Keyword(s):  
Density Distribution ◽  
Surface Density ◽  
Solar Nebula

scholarly journals Photophoresis in the circumjovian disk and its impact on the orbital configuration of the Galilean satellites

2019 ◽  
Vol 629 ◽  
pp. A106 ◽  
Author(s):  
Sota Arakawa ◽  
Yuhito Shibaike
Keyword(s):  
Density Distribution ◽  
Accretion Disks ◽  
Surface Density ◽  
Outer Region ◽  
Dust Particles ◽  
Magnetorotational Instability ◽  
Galilean Satellites ◽  
Ionization Fraction ◽  
Orbital Configuration ◽  
Inner Region

Jupiter has four large regular satellites called the Galilean satellites: Io, Europa, Ganymede, and Callisto. The inner three of the Galilean satellites orbit in a 4:2:1 mean motion resonance; therefore their orbital configuration may originate from the stopping of the migration of Io near the bump in the surface density distribution and following resonant trapping of Europa and Ganymede. The formation mechanism of the bump near the orbit of the innermost satellite, Io, is not yet understood, however. Here, we show that photophoresis in the circumjovian disk could be the cause of the bump using analytic calculations of steady-state accretion disks. We propose that photophoresis in the circumjovian disk could stop the inward migration of dust particles near the orbit of Io. The resulting dust-depleted inner region would have a higher ionization fraction, and thus admit increased magnetorotational-instability-driven accretion stress in comparison to the outer region. The increase of the accretion stress at the photophoretic dust barrier would form a bump in the surface density distribution, halting the migration of Io.

The effects of surface topography of nanostructure arrays on cell adhesion

2018 ◽  
Vol 20 (35) ◽  
pp. 22946-22951 ◽  
Author(s):  
Jing Zhou ◽  
Xiaowei Zhang ◽  
Jizheng Sun ◽  
Zechun Dang ◽  
Jinqi Li ◽  
...  
Keyword(s):  
Cell Adhesion ◽  
Density Distribution ◽  
Surface Topography ◽  
Thermodynamic Model ◽  
Surface Density ◽  
Distribution Density ◽  
Small Radius ◽  
Surface Distribution ◽  
Nanostructure Arrays

The effects of geometry and surface density distribution of nanopillars on cell adhesion studied by a quantitative thermodynamic model showed that high (low) surface distribution density and large (small) radius result in the “Top” (“Bottom”) mode.

scholarly journals 3.17. MACHO RR Lyrae stars in the Galactic bulge: the spatial distribution

1998 ◽  
Vol 184 ◽  
pp. 123-124
Author(s):  
D. Minniti ◽  
C. Alcock ◽  
D. Alves ◽  
K. Cook ◽  
S. Marshall ◽  
...  
Keyword(s):  
Spatial Distribution ◽  
Density Distribution ◽  
Surface Density ◽  
Galactic Bulge ◽  
Rr Lyrae Stars ◽  
Rr Lyrae ◽  
Type C ◽  
Type Ab ◽  
Lyrae Stars

We have analyzed a sample of 1150 type ab, and 550 type c RR Lyrae stars found in 24 of 94 bulge fields of the MACHO database. These fields cover a range in Galactocentric distances from 0.3 to 1.6 kpc. In combination with the data on the outer bulge fields of Alard (1997) and Wesselink (1987), here we present the surface density distribution of bulge RR Lyrae between 0.3 and 3 kpc.

scholarly journals M-dwarf exoplanet surface density distribution

2018 ◽  
Vol 612 ◽  
pp. L3 ◽  
Author(s):  
Michael R. Meyer ◽  
Adam Amara ◽  
Maddalena Reggiani ◽  
Sascha P. Quanz
Keyword(s):  
Density Distribution ◽  
Surface Density ◽  
Probability Distributions ◽  
Mass Range ◽  
Normal Function ◽  
Point Estimates ◽  
Points Of View ◽  
Log Normal ◽  
Parameter Values ◽  
M Dwarf

Aims. We fit a log-normal function to the M-dwarf orbital surface density distribution of gas giant planets, over the mass range 1–10 times that of Jupiter, from 0.07 to 400 AU. Methods. We used a Markov chain Monte Carlo approach to explore the likelihoods of various parameter values consistent with point estimates of the data given our assumed functional form. Results. This fit is consistent with radial velocity, microlensing, and direct-imaging observations, is well-motivated from theoretical and phenomenological points of view, and predicts results of future surveys. We present probability distributions for each parameter and a maximum likelihood estimate solution. Conclusions. We suggest that this function makes more physical sense than other widely used functions, and we explore the implications of our results on the design of future exoplanet surveys.

scholarly journals Ice lines, planetesimal composition and solid surface density in the solar nebula

Icarus ◽  
2009 ◽  
Vol 200 (2) ◽  
pp. 672-693 ◽  
Author(s):  
Sarah E. Dodson-Robinson ◽  
Karen Willacy ◽  
Peter Bodenheimer ◽  
Neal J. Turner ◽  
Charles A. Beichman
Keyword(s):  
Solid Surface ◽  
Surface Density ◽  
Solar Nebula

scholarly journals Simultaneous formation of Jupiter and Saturn

2010 ◽  
Vol 6 (S276) ◽  
pp. 428-429
Author(s):  
Octavio M. Guilera ◽  
Adrián Brunini ◽  
Omar G. Benvenuto
Keyword(s):  
Density Distribution ◽  
Solar Nebula ◽  
Classical Model ◽  
Protoplanetary Disk ◽  
Instability Mechanism ◽  
Simultaneous Formation ◽  
The Core ◽  
Growth Regime ◽  
Significant Change

AbstractWe calculate the simultaneous in situ formation of Jupiter and Saturn by the core instability mechanism considering the oligarchic growth regime for the accretion of planetesimals. We consider a density distribution for the size of planetesimals and planetesimals migration. The planets are immersed in a realistic protoplanetary disk that evolves with time. We find that, within the classical model of solar nebula, the isolated formation of Jupiter and Saturn undergoes significant change when it occurs simultaneously.

SNR Surface Density Distribution in Nearby Galaxies

2004 ◽  
Vol 289 (3/4) ◽  
pp. 283-286 ◽  
Author(s):  
Manami Sasaki ◽  
Dieter Breitschwerdt ◽  
Rodrigo Supper
Keyword(s):  
Density Distribution ◽  
Surface Density ◽  
Nearby Galaxies

Measurement of surface-density distribution in moving sheet materials by means of local translucence method

1976 ◽  
Vol 19 (12) ◽  
pp. 1739-1741
Author(s):  
V. V. Summovskii ◽  
A. A. Adamenko ◽  
V. N. Momot
Keyword(s):  
Density Distribution ◽  
Surface Density ◽  
Sheet Materials

scholarly journals Jupiter formed as a pebble pile around the N2 ice line

2019 ◽  
Vol 632 ◽  
pp. L11 ◽  
Author(s):  
A. D. Bosman ◽  
A. J. Cridland ◽  
Y. Miguel
Keyword(s):  
Surface Density ◽  
Total Mass ◽  
Planet Formation ◽  
Solar Nebula ◽  
Heavy Elements ◽  
Oxygen Abundance ◽  
The Core ◽  
Nitrogen Abundance ◽  
The Ideal

Context. The region around the H2O ice line, due to its higher surface density, seems to be the ideal location to form planets. The core of Jupiter, as well as the cores of close-in gas giants are therefore thought to form in this region of the disk. Nevertheless, constraining the formation location of individual planets has proven to be difficult. Aims. We aim to use the nitrogen abundance in Jupiter, which is around four times solar, in combination with Juno constraints on the total mass of heavy elements in Jupiter to narrow down its formation scenario. Methods. Different pathways of enrichment of the atmosphere of Jupiter are considered, such as the accretion of enriched gas, pebbles, and planetesimals, and their implications for the oxygen abundance of Jupiter are discussed. Results. The super-solar nitrogen abundance in Jupiter necessitates the accretion of extra N2 from the proto-solar nebula. The only location of the disk where this can happen is outside or just inside the N2 ice line. These constraints favor a pebble accretion origin of Jupiter, from the perspective of composition and planet formation. We predict that Jupiter’s oxygen abundance is between 3.6 and 4.5 times solar.

scholarly journals The potential of combining MATISSE and ALMA observations: constraining the structure of the innermost region in protoplanetary discs

2019 ◽  
Vol 622 ◽  
pp. A147 ◽  
Author(s):  
J. Kobus ◽  
S. Wolf ◽  
R. Brunngräber
Keyword(s):  
Density Distribution ◽  
Surface Density ◽  
Initial Conditions ◽  
Central Star ◽  
Nearby Star ◽  
Dust Density ◽  
Star Forming ◽  
The Impact ◽  
Innermost Region ◽  
Protoplanetary Discs

Context. In order to study the initial conditions of planet formation, it is crucial to obtain spatially resolved multi-wavelength observations of the innermost region of protoplanetary discs. Aims. We evaluate the advantage of combining observations with MATISSE/VLTI and ALMA to constrain the radial and vertical structure of the dust in the innermost region of circumstellar discs in nearby star-forming regions. Methods. Based on a disc model with a parameterized dust density distribution, we apply 3D radiative-transfer simulations to obtain ideal intensity maps. These are used to derive the corresponding wavelength-dependent visibilities we would obtain with MATISSE as well as ALMA maps simulated with CASA. Results. Within the considered parameter space, we find that constraining the dust density structure in the innermost 5 au around the central star is challenging with MATISSE alone, whereas ALMA observations with reasonable integration times allow us to derive significant constraints on the disc surface density. However, we find that the estimation of the different disc parameters can be considerably improved by combining MATISSE and ALMA observations. For example, combining a 30-min ALMA observation (at 310 GHz with an angular resolution of 0.03′′) for MATISSE observations in the L and M bands (with visibility accuracies of about 3%) allows the radial density slope and the dust surface density profile to be constrained to within Δα = 0.3 and Δ(α − β) = 0.15, respectively. For an accuracy of ~1% even the disc flaring can be constrained to within Δβ = 0.1. To constrain the scale height to within 5 au, M band accuracies of 0.8% are required. While ALMA is sensitive to the number of large dust grains settled to the disc midplane we find that the impact of the surface density distribution of the large grains on the observed quantities is small.

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