Table 1
Best-fit model physical parameters for the molecular region of NGC 6302.
Structure | δ V | n | T | V exp | Age | M |
(km s-1) | (104 cm-3) | (K) | (km s-1) | (1000 yr) | (M⊙) | |
|
||||||
Inner ring | linear,Vmax | |||||
|
||||||
IR | 2 | 14![]() |
50![]() |
11![]() |
2.2 | 2.7 × 10-3 |
|
||||||
Main ring (inner region) | constant | |||||
|
||||||
MR-B1 | 1 | 35![]() |
260![]() |
8![]() |
3.5−3.8 | 1.1 × 10-2 |
MR-R1 | 2 | 60![]() |
200![]() |
11![]() |
2.5−2.7 | 2 × 10-2 |
|
||||||
Main ring (outer region) | n range | linear,Vmax | ||||
|
||||||
MR-B2 | 2 | (16.2−12.2)![]() |
40![]() |
13.1![]() |
2.9 | 4.7 × 10-2 |
MR-R2 | 2 | (7.5−5.7)![]() |
40![]() |
10.4![]() |
3.7 | 1 × 10-2 |
MR-R3 | 2 | (0.9−0.7)![]() |
180![]() |
14.4![]() |
3.7 | 1.4 × 10-4 |
|
||||||
Lobe fragments | n range | linear,Vmax | ||||
|
||||||
LF-B1 | 2 | (2.9−1.5)![]() |
40![]() |
17![]() |
4.3 | 2.1 × 10-3 |
LF-B2 | 2 | (5.6−3)![]() |
80![]() |
24.1![]() |
3.1 | 4.4 × 10-3 |
LF-B3 | 2 | (2.1−1.4)![]() |
40![]() |
13.1![]() |
4.6 | 7.9 × 10-4 |
LF-B4 | 2 | (2.1−1.3)![]() |
40![]() |
14.2![]() |
4.6 | 6.5 × 10-4 |
LF-B5 | 2 | (1−0.35)![]() |
40![]() |
20.5![]() |
5.1 | 1 × 10-3 |
LF-B6 | 2 | (4.3−3.3)![]() |
40![]() |
12.3![]() |
4.1 | 1.1 × 10-3 |
LF-R1 | 2 | (0.7−0.5)![]() |
40![]() |
11.8![]() |
5.1 | 6.2 × 10-4 |
LF-R2 | 2 | (1.7−1)![]() |
40![]() |
17.6![]() |
3.7 | 1.2 × 10-3 |
Notes. For the structure labelling and the geometric shape of each structure, refer to Fig. 4 or to the model file in SHAPE format available at the CDS. Parameters: δV is the characteristic microturbulence velocity of the structure. n is the density of the structure. When only one value is shown, the density is constant across the structure. When a range of values is shown, the density falls with the inverse of the distance to the star, and the values shown reflect the maximum and minimum density of the given structure. T is the temperature of the structure. Vexp is the expansion velocity. In the case of the inner region of the main ring, it is a constant value. In every other case, the value of the velocity shown corresponds to the farthest edge of the structure from the star, with the velocity following a linear, ballistic expansion pattern. Age refers to the kinematical age of the structure, and M to its mass.
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