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Minor cleaup

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Alexander Bock
2020-09-16 23:07:32 +02:00
parent 2a4ad44740
commit dffa7b914a
2 changed files with 37 additions and 42 deletions
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29
data/assets/scene/milkyway/objects/orionnebula/cluster.asset
View File

@@ -32,22 +32,19 @@ assetHelper.registerSceneGraphNodesAndExport(asset, { OrionClusterStars })
asset.meta = {
Name = "Orion Nebula Star Cluster",
Version = "1.0",
Description = [[ In order to have an accurate depiction of the
Orion nebula, we need to include the star cluster that was birthed
from it. We turned to a study of the cluster’s stellar population by
Lynne Hillenbrand, who was working at the University of California, Berkeley at
the time.The catalog from her paper contains more than 1,500 stars, about
half the stars in the actual cluster. The cluster is very crowded, with
a peak density of 10,000 stars per cubic parsec over a wide range
of masses from a tenth the sun’s mass up to 50 times its mass. We
were presented with one problem: there are no distances.
For the stellar distances, we needed to deduce them by statistical
methods. Knowing the size of the cluster and approximating the
shape to be roughly spherical, we placed each star along a line
of sight through this imaginary sphere centered on the cluster. In
this sense, these data are observed data and the view from Earth is
accurate. But the distance of each star has been derived from this
educated-guess approach for the cluster distribution. ]],
Description = [[ In order to have an accurate depiction of the Orion nebula, we need
to include the star cluster that was birthed from it. We turned to a study of the
cluster's stellar population by Lynne Hillenbrand, who was working at the University of
California, Berkeley at the time. The catalog from her paper contains more than 1500
stars, about half the stars in the actual cluster. The cluster is very crowded, with a
peak density of 10000 stars per cubic parsec over a wide range of masses from a tenth the
sun's mass up to 50 times its mass. We were presented with one problem: there are no
distances. For the stellar distances, we needed to deduce them by statistical methods.
Knowing the size of the cluster and approximating the shape to be roughly spherical, we
placed each star along a line of sight through this imaginary sphere centered on the
cluster. In this sense, these data are observed data and the view from Earth is accurate.
But the distance of each star has been derived from this educated-guess approach for the
cluster distribution. ]],
Author = "AMNH Digital Universe",
URL = "https://www.amnh.org/research/hayden-planetarium/digital-universe",
License = "custom"

50
data/assets/scene/milkyway/objects/orionnebula/nebula.asset
View File

@@ -27,7 +27,7 @@ local NebulaHolder = {
XAxisOrthogonal = true,
YAxis = "Sun",
YAxisInverted = false
}
}
},
GUI = {
Name = "Orion Nebula",
@@ -51,12 +51,12 @@ local OrionNebulaModel = {
GeometryFile = sync .. "/orion_nebula.obj",
ColorTexture = sync .. "/heic0601a_masked.png"
}},
Opacity = 1.0,
Opacity = 1.0,
DisableFaceCulling = false,
SpecularIntensity = 0.0,
AmbientIntensity = 0.45,
SpecularIntensity = 0.0,
AmbientIntensity = 0.45,
DiffuseIntensity = 0.0,
RotationVector = {0.000000, 22.300000, 0.000000},
RotationVector = { 0.000000, 22.300000, 0.000000 },
LightSources = LIGHTS;
},
GUI = {
@@ -84,10 +84,10 @@ local OrionNebulaShocksModel = {
}},
Opacity = 1.0,
DisableFaceCulling = false,
SpecularIntensity = 0.0,
AmbientIntensity = 0.19,
SpecularIntensity = 0.0,
AmbientIntensity = 0.19,
DiffuseIntensity = 0.4,
RotationVector = {0.000000, 22.300000, 0.000000},
RotationVector = { 0.000000, 22.300000, 0.000000 },
LightSources = LIGHTS;
},
GUI = {
@@ -115,10 +115,10 @@ local OrionNebulaProplydsModel = {
}},
Opacity = 1.0,
DisableFaceCulling = false,
SpecularIntensity = 0.0,
AmbientIntensity = 1.0,
SpecularIntensity = 0.0,
AmbientIntensity = 1.0,
DiffuseIntensity = 1.0,
RotationVector = {0.000000, 22.300000, 0.000000},
RotationVector = { 0.000000, 22.300000, 0.000000 },
LightSources = LIGHTS;
},
GUI = {
@@ -138,21 +138,19 @@ assetHelper.registerSceneGraphNodesAndExport(asset, {
asset.meta = {
Name = "Orion Nebula Model",
Version = "1.0",
Description = [[ In the Digital Universe model of the Orion Nebula,
we depict the ionization front effectively as a terrain, with a flat Hubble
image of the nebula mapped on the undulating surface. In
reality, the ionization front has a slight thickness to it - about a third
of a light year - but is quite thin compared to the overall size of the
nebula, which stretches about ten light years from side to side.<br><br>Close into
the center, we see small teardrop-shaped structures with their
narrow ends pointing away from the bright star: these are protoplanetary
disks, or proplyds, of dense gas and dust surrounding young stars. The larger
formations that one sees farther away from the center of the nebula take on a
cup-like shape, with the narrow end pointing away from the nebulas center.
These enormous structures are bow shocks that delineate the region where
highspeed winds from the central star slow from supersonic to subsonic speeds.
You can think of an Hii region as a sort of tremendous explosion, taking place
over millennia, and the bow shocks are part of the outward rush of material. ]],
Description = [[ In the Digital Universe model of the Orion Nebula, we depict the
ionization front effectively as a terrain, with a flat Hubble image of the nebula mapped
on the undulating surface. In reality, the ionization front has a slight thickness to
it - about a third of a light year - but is quite thin compared to the overall size of
the nebula, which stretches about ten light years from side to side.<br><br>Close into
the center, we see small teardrop-shaped structures with their narrow ends pointing away
from the bright star: these are protoplanetary disks, or proplyds, of dense gas and dust
surrounding young stars. The larger formations that one sees farther away from the center
of the nebula take on a cup-like shape, with the narrow end pointing away from the
nebulas center. These enormous structures are bow shocks that delineate the region where
highspeed winds from the central star slow from supersonic to subsonic speeds. You can
think of an HII region as a sort of tremendous explosion, taking place over millennia,
and the bow shocks are part of the outward rush of material. ]],
Author = "AMNH Digital Universe",
URL = "https://www.amnh.org/research/hayden-planetarium/digital-universe",
License = "custom"