Version 175 (modified by 10 years ago) ( diff ) | ,
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Link to Jonathan's Paper: The Effects of Inhomogeneities within Colliding Flows on the Formation and Evolution of Molecular Clouds
Individual Run Views
Shear 0
Shear 0
Column Density Map with Sinks (left)
In corrected units of n (cm-2)
Inverse Beta Maps (right)
Made by projecting the quantity, inverse beta, through the grid.
Sinks
Total = 4.
x-coordinate (pc) | y-coordinate (pc) | z-coordinate (pc) | Frame first formed (Chombo No.) | Time first formed (Myr) | Mass at 27.3 Myr (Solar Masses) |
35.8 | 55.8 | 47.45 | 111 | 10.989 | 178 |
35.92 | 56 | 47.56 | 120 | 11.88 | 38.9 |
35.92 | 56.02 | 47.6 | 138 | 13.662 | 20.7 |
44.67 | 38.12 | 29.8 | 236 | 23.364 | 109 |
B vs. n
The gray scale is for the thermal pressure vs density plots, and the color scale is the magnetic pressure vs. density plots. The line is T=10K, dotted line = ram pressure of the flows, and dashed line = initial magnetic pressure.
Spectra
Gravitational energy spectra made by taking the Fourier Transform of Sqrt(-gravitational_energy) to avoid nans, since the gravitational energy was everywhere negative.
Time Evolution View | Energy Evolution View |
E vs. t Plots
These are all plots of bulk energy in the collision region over time.
This plot shows each of the energies (grav., mag., kinetic), divided by the initial kinetic energy in the collision region. It shows that the dominant energy in the collision region is kinetic.
This plot shows each of the energies (grav., mag., kinetic), divided by their own initial values, showing how much each of the energies change over time. It shows that the gravitational energy has the steepest growth rate of these 3 energies. The curve reaches a peak plateau at about 10 Myr, coinciding with the formation of the first sink.
This plot shows each of the energies (grav., mag.), divided by the kinetic energy at each time; it is an instantaneous view of the ratio of these energies to the kinetic energy in the collision region. It shows that after the steep growth in gravitational energy (after 10 Myr), the gravitational energy remains only at about 25% the kinetic. The magnetic energy remains a much smaller fraction throughout the simulation.
Streamline Plots (Global vs. local views)
Some example streamline plots
Streamline Global View
Shear 15
Shear 15
Column Density Map with Sinks (left) & Inverse Beta Maps (right)
Sink Notes:
- The number of the sinks that form by the end of this simulate is 4.
- Here are their positions as seen down the barrel of the flow (see mass1 CDM plots) at final frame:
x-coordinate (pc) | y-coordinate (pc) | z-coordinate (pc) | Frame first formed (Chombo No.) | Time (Myr) | Mass at 27.3 Myr (Solar Masses) |
13.06 | 35.81 | 41.29 | 181 | 17.919 | 49.1 |
29.37 | 28.59 | 49.8 | 203 | 20.097 | 19.9 |
10.9 | 33.76 | 39.51 | 240 | 23.736 | 45 |
12.07 | 33.88 | 50.17 | 264 | 26.11 | 11.2 |
8.44 | 35.11 | 39.53 | 268 | 26.51 | 6.45 |
B vs. n
The gray scale is for the thermal pressure vs density plots, and the color scale is the magnetic pressure vs. density plots. The line is T=10K, dotted line = ram pressure of the flows, and dashed line = initial magnetic pressure.
Spectra
Gravitational energy spectra made by taking the Fourier Transform of Sqrt(-gravitational_energy) to avoid nans, since the gravitational energy was everywhere negative.
Time Evolution View | Energy Evolution View |
Streamline Global View
Shear 30
Shear 30
Column Density Map with Sinks (left) & Inverse Beta Maps (right)
Sink Notes:
- The number of the sinks that form by the end of this simulate is 1.
- Here is its position as seen down the barrel of the flow (see mass1 CDM plots) at final frame:
x-coordinate (pc) | y-coordinate (pc) | z-coordinate (pc) | Frame first formed (Chombo No.) | Time (Myr) | Mass at 27.3 Myr (Solar Masses) |
103.23 | 40.05 | 33.8 | 138 | 13.662 | 11.3 |
B vs. n
The gray scale is for the thermal pressure vs density plots, and the color scale is the magnetic pressure vs. density plots. The line is T=10K, dotted line = ram pressure of the flows, and dashed line = initial magnetic pressure.
Spectra
Gravitational energy spectra made by taking the Fourier Transform of Sqrt(-gravitational_energy) to avoid nans, since the gravitational energy was everywhere negative.
Time Evolution View | Energy Evolution View |
Streamline Global View
Shear 60
Shear 60
Column Density Map with Sinks (left) & Inverse Beta Maps (right)
Sink Notes:
- The number of the sinks that form by the end of this simulate is 1.
- Here is its position as seen down the barrel of the flow (see mass1 CDM plots) at final frame:
x-coordinate (pc) | y-coordinate (pc) | z-coordinate (pc) | Frame first formed (Chombo No.) | Time (Myr) | Mass at 32.7 Myr (Solar Masses) |
104.13 | 49.1 | 36.1 | 320 | 31.68 | 14.4 |
B vs. n
The gray scale is for the thermal pressure vs density plots, and the color scale is the magnetic pressure vs. density plots. The line is T=10K, dotted line = ram pressure of the flows, and dashed line = initial magnetic pressure.
Spectra
Gravitational energy spectra made by taking the Fourier Transform of Sqrt(-gravitational_energy) to avoid nans, since the gravitational energy was everywhere negative.
Time Evolution View | Energy Evolution View |
Streamlines Global View
Table Comparison Views
Sink Information
Sink Information
Charts
Figure 1. The blue & right hand vertical axis indicates the total mass in solar masses (i.e. summation of all the masses) of the sinks in that particular run series by the final frame. The red & right hand vertical axis measures the number of sinks that formed in total for that run series. Note that Shear 60 is the only run that did not form a sink before 27.3 Myr (rather 32.8 Myr). BW Version |
Figure 2. The individual masses and formation times of the cores formed for each run series as denoted by the different colors. The sinks are numbered and colored by order of formation. One can see that they add up to the total mass illustrated in Figure 1. BW Version |
Figure 3. A column chart that indicates the number of sinks that form that are binned for 0-10, 10-100, and 100-1000 solar masses for each run. The runs are illustrated by color. |
Spectra Tables
Column Density & Inverse Beta Maps
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CFMeetingNotes.pdf
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For 12-18-2014
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