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

Down y-axis global view

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

Streamline Plots

Streamline Plots

Streamline Plot of 3 Runs

Sink Information

Sink Information

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. ​BW Version

Shear 0

Mass information on sinks, mass in the box, and collision region.

Spectra Tables

Spectra Tables

Spectra Table: Energies vs. Time

Spectra Table: Run vs. Time

Spectra Table: Run vs. Energy

Column Density & Inverse Beta Maps

Column Density & Inverse Beta Maps

	​Column Density Map with Sinks (left) ​Inverse Beta Maps (right)
Shear 0
Shear 15
Shear 30
Shear 60

B vs. n

B vs. n Plots

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.

Shear 0
Shear 15
Shear 30
Shear 60