by johnnydeep » Thu Jun 27, 2024 6:34 pm
Yeah, I'm not clearly seeing any obvious aligned "jests" in this image. Fortunately, there is a nice image at the "detailed explanation"
link that provides some help, though the alignments aren't as close as I was expecting. The original image is too big to post, but here's a side-by-side comparison with today's APOD:
Figure 1:The central location of each outflow (green arrows) and suggested driving sources (blue stars) indicated on a NIRCam-color image (F140M - blue, F210M - green, F360M - orange, F480M - red). The arrow and source locations are offset from the outflow for clarity - refer to the coordinates in the catalogue for accurate outflow coordinates. This combined image is centered at approximately 18:29:55.8 +01:14:34. Image processing credit: Alyssa Pagan.
The spin axes of very young stars may be efficiently traced by their outflows. Indeed, the emergence of energetic protostellar outflows is a ubiquitous signature of early star formation (Frank et al., 2014). Collimated jets launching from the innermost regions of low-mass young stars impact surrounding molecular cloud material and can create striking structures of shocked ionized, atomic, and molecular gas (Reipurth & Bally, 2001; Bally, 2016). Since the jets are likely accelerated and collimated by a rapidly rotating poloidal magnetic field in the inner star-disk system, they emerge along the stellar rotation axis and thus trace the angular momentum vector of the star itself (Kwan & Tademaru, 1988; Ouyed & Pudritz, 1997; Banerjee & Pudritz, 2006).
Jet material ejected from protostellar systems may contain sufficient momentum to reach distances comparable to the entire cloud, giving rise to spectacular “parsec-scale” outflows (Eisloffel & Mundt, 1997; Reipurth et al., 1997). As some protostellar outflows traverse molecular cloud core scales (
∼
1-2 pc) in less than the cloud life time, they provide an important feedback mechanism that may act to limit the ability of a cloud to form new stars (Hansen et al., 2012; Plunkett et al., 2015). Indeed, molecular clouds are known to form stars at a relatively low conversion efficiency (Evans et al., 2009; Federrath & Klessen, 2012).
Yeah, I'm not clearly seeing any obvious aligned "jests" in this image. Fortunately, there is a nice image at the "detailed explanation" [url=https://arxiv.org/html/2406.13084v1]link[/url] that provides some help, though the alignments aren't as close as I was expecting. The original image is too big to post, but here's a side-by-side comparison with today's APOD:
[attachment=0]Protostellar Outflows in Serpens.jpg[/attachment]
[quote][b]Figure 1[/b]:The central location of each outflow (green arrows) and suggested driving sources (blue stars) indicated on a NIRCam-color image (F140M - blue, F210M - green, F360M - orange, F480M - red). The arrow and source locations are offset from the outflow for clarity - refer to the coordinates in the catalogue for accurate outflow coordinates. This combined image is centered at approximately 18:29:55.8 +01:14:34. Image processing credit: Alyssa Pagan.
The spin axes of very young stars may be efficiently traced by their outflows. Indeed, the emergence of energetic protostellar outflows is a ubiquitous signature of early star formation (Frank et al., 2014). Collimated jets launching from the innermost regions of low-mass young stars impact surrounding molecular cloud material and can create striking structures of shocked ionized, atomic, and molecular gas (Reipurth & Bally, 2001; Bally, 2016). Since the jets are likely accelerated and collimated by a rapidly rotating poloidal magnetic field in the inner star-disk system, they emerge along the stellar rotation axis and thus trace the angular momentum vector of the star itself (Kwan & Tademaru, 1988; Ouyed & Pudritz, 1997; Banerjee & Pudritz, 2006).
Jet material ejected from protostellar systems may contain sufficient momentum to reach distances comparable to the entire cloud, giving rise to spectacular “parsec-scale” outflows (Eisloffel & Mundt, 1997; Reipurth et al., 1997). As some protostellar outflows traverse molecular cloud core scales (
∼
1-2 pc) in less than the cloud life time, they provide an important feedback mechanism that may act to limit the ability of a cloud to form new stars (Hansen et al., 2012; Plunkett et al., 2015). Indeed, molecular clouds are known to form stars at a relatively low conversion efficiency (Evans et al., 2009; Federrath & Klessen, 2012).[/quote]