scispace - formally typeset
Search or ask a question

Where in the Milky Way do we see star formation happening? 

Answers from top 6 papers

More filters
Papers (6)Insight
A dedicated, deep survey of nearby galaxies provides a snapshot of their recent star formation, shedding new light on the process of star formation and its modalities in different environments and conditions.
That burst of star formation must have been particularly spectacular and may be related to the activity we now see in the distant blue dwarf galaxies revealed in deep imaging.
This strongly suggests that star formation in the Milky Way is a dynamic process on GMC scales.
Consistently, the statistical analysis of positions and ages of clusters in the Milky Way disk strongly suggests that a correlation between the duration of star formation in a region and its size does exist.
We do not find a correlation between the recent star-formation activity and the distance to the nearest neighboring galaxy, suggesting that the star-formation process is not driven by gravitational interactions, but regulated internally.
We suggest that the phenomena revealed here support a scenario of hierarchical star formation.

See what other people are reading

What evidence is there for how the star systems formed?
4 answers
What are RS CVn stars?
5 answers
What are RS CVn stars?
5 answers
Can star at halo trace dark matter distribution?
5 answers
Yes, stars in a halo can indeed trace the distribution of dark matter (DM). Research shows that the stellar surface brightness and globular clusters (GCs) in a halo closely correspond to the distribution of DM and total mass, allowing for an accurate recovery of the DM profile from stars and GCs. The method is robust even in the presence of satellites and improves with fainter GC samples. Additionally, the radial profiles of GC populations, combined with galaxy mass, can effectively trace the density profile of the DM halo, providing insights into the structural properties of the DM haloes of galaxies, even beyond the Local Group. Therefore, stars and GCs in a halo can be valuable tools for studying and constraining the underlying distribution of dark matter.
What is the dark matter radial profile of milky way?
5 answers
The dark matter radial profile of the Milky Way has been extensively studied using various methods. Recent research has shown that the Milky Way's dark matter density profile can be better described by a cored Einasto profile with a slope parameter of $0.91^{+0.04}_{-0.05}$, rather than a generalized Navarro-Frenk-White (NFW) profile. Additionally, investigations utilizing cosmological simulations have highlighted the importance of the "splashback" radius in delineating the outer boundary of the dark matter halo, with significant scatter observed in the velocity dispersion profiles of dark and luminous tracers within Milky Way-mass halos. Furthermore, a non-parametric method has been developed to directly infer the dark matter contribution to the circular velocity across the Galaxy, allowing for a clean determination of the dark matter profile without theoretical bias.
What are the properties of the pulse-driven convective zone in AGB Stars?
5 answers
The pulse-driven convective zone in Asymptotic Giant Branch (AGB) stars exhibits significant mixing processes influenced by convective boundary mixing (CBM). Hydrodynamic simulations suggest the presence of CBM at the bottom of the thermal pulse-driven convective zone, impacting the He-intershell abundances of 12C and 16O. This mixing affects the activation of 22Ne(α,n)25Mg and the efficiency of the s-process in the 13C-pocket of AGB stars. The convective boundary mixing at the base of the pulse-driven convection zone is crucial for understanding the nucleosynthesis processes and the overall evolution of AGB stars.
What is the galactic coordinate of the orion arm?
5 answers
The Galactic coordinate of the Orion arm is characterized by a narrow ellipsoid elongated in the direction of L1 = 77.1° ± 2.9°, with a symmetry plane inclined at an angle of 5.6° ± 0.2° to the Galactic plane. The longitude of the ascending node of this symmetry plane is approximately \(l_\Omega = 70^\circ \pm 3^\circ\). Additionally, the pitch angle of the Local spiral arm is estimated to be i = 12.9° ± 2.9°. This orientation is further supported by the absence of a deviation from the direction to the Galactic pole in the third axis of the position ellipsoid of Galactic masers. The Orion arm is a significant feature in the Milky Way, hosting star-forming complexes and playing a crucial role in the structure and dynamics of our galaxy.
Role of volume in gas law?
5 answers
Volume plays a crucial role in various gas laws and their applications. In the context of star formation laws, volume densities of gas (HI+H2) in galaxies exhibit a tight correlation with the star formation rate (SFR), emphasizing the importance of considering three-dimensional density profiles by accounting for the radial growth of gaseous discs. Additionally, in the study of heat radiation from gas volumes, the laws of radiation from gas volumes have been shown to impact fuel saving and environmental pressure reduction by considering the dimensions, power, and geometrical position of radiative gas volumes, highlighting the significance of volume in heat transfer calculations. Therefore, understanding and incorporating volume measurements are essential in various fields to comprehend and predict the behavior of gases accurately.
List 6 advantages of group dating?
5 answers
Group dating offers several advantages, as supported by the data from various contexts. Firstly, group sex participation among heterosexual individuals can provide a sense of safety and comfort, reducing the risk of STIs through shared awareness and support in practicing safe sex behaviors. Secondly, in social scenarios like dating, group dynamics can enhance confidence levels among individuals, making interactions more relaxed and enjoyable, potentially leading to better connections and relationships. Additionally, group dating can facilitate risk assessment and informed decision-making regarding sexual activities, contributing to a more responsible approach to dating and intimacy. Furthermore, group settings can offer a diverse range of perspectives and experiences, enriching social interactions and fostering a sense of community and belonging. Lastly, group dating can help in exploring different social venues and meeting new people, broadening one's social circle and enhancing social skills.
What does the Cheshire Cat represent in Alice's unconsciousness as a feeling or emotion?
5 answers
The Cheshire Cat in Lewis Carroll's "Alice's Adventures in Wonderland" symbolizes various concepts across different contexts. In the context of modern normative decision theory, the Cheshire Cat provides clear and simple advice, highlighting significant tenets often overlooked in engineering design. Additionally, the quantum Cheshire cat effect, inspired by the dis-embodied grin of the Cheshire Cat, is a phenomenon in quantum theory where a particle's properties can be separated from its location through weak probing, as demonstrated with photons and neutrons in experiments. Furthermore, in a creative context, the Cheshire Cat metaphorically represents 'madness' and the dominance of the unconscious in the artistic process, as articulated by Lewis Carroll, influencing the works of various artists. Thus, the Cheshire Cat embodies advice, quantum phenomena, and artistic inspiration, reflecting a multifaceted symbol in different realms.
What is the small things to study the universe ?
4 answers
Studying the universe involves investigating a wide range of celestial objects and phenomena, from dwarf irregular galaxies to ultrafaint dwarf galaxies, cosmic expansion, and even the distribution of dark matter using strongly lensed systems. Dwarf irregular galaxies provide insights into total matter distribution, while ultrafaint dwarf galaxies offer a glimpse into early galaxy formation. Cosmic expansion, likened to a balloon's surface expanding, is a fundamental concept explored theoretically and experimentally. Additionally, the distribution of dark matter on small scales can be probed through the unique anisotropic signature in the lensing deflection field due to line-of-sight halos. These small-scale studies contribute significantly to our understanding of the universe's dynamics, evolution, and composition.