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Journal articles on the topic 'Star-forming'

Author: Grafiati
Published: 4 June 2021
Last updated: 7 February 2022

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1

Kaifu, Norio. "Star forming regions." Vistas in Astronomy 31 (1988): 199–206. http://dx.doi.org/10.1016/0083-6656(88)90202-4.

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2

Ivison, R. J., J. Richard, A. D. Biggs, M. A. Zwaan, E. Falgarone, V. Arumugam, P. P. van der Werf, and W. Rujopakarn. "Giant star-forming clumps?" Monthly Notices of the Royal Astronomical Society: Letters 495, no. 1 (March 16, 2020): L1—L6. http://dx.doi.org/10.1093/mnrasl/slaa046.

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ABSTRACT With the spatial resolution of the Atacama Large Millimetre Array (ALMA), dusty galaxies in the distant Universe typically appear as single, compact blobs of dust emission, with a median half-light radius, ≈1 kpc. Occasionally, strong gravitational lensing by foreground galaxies or galaxy clusters has probed spatial scales 1–2 orders of magnitude smaller, often revealing late-stage mergers, sometimes with tantalizing hints of sub-structure. One lensed galaxy in particular, the Cosmic Eyelash at z = 2.3, has been cited extensively as an example of where the interstellar medium exhibits obvious, pronounced clumps, on a spatial scale of ≈100 pc. Seven orders of magnitude more luminous than giant molecular clouds in the local Universe, these features are presented as circumstantial evidence that the blue clumps observed in many z ∼ 2–3 galaxies are important sites of ongoing star formation, with significant masses of gas and stars. Here, we present data from ALMA which reveal that the dust continuum of the Cosmic Eyelash is in fact smooth and can be reproduced using two Sérsic profiles with effective radii, 1.2 and 4.4 kpc, with no evidence of significant star-forming clumps down to a spatial scale of ≈80 pc and a star formation rate of <3 M⊙ yr−1.
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3

Myers, Philip C. "Star-forming Filament Models." Astrophysical Journal 838, no. 1 (March 17, 2017): 10. http://dx.doi.org/10.3847/1538-4357/aa5fa8.

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4

Álvarez-Álvarez, Mar, Ángeles I. Díaz, and Marcelo Castellanos. "Massive star population in circumnuclear star-forming regions." Symposium - International Astronomical Union 212 (2003): 537–38. http://dx.doi.org/10.1017/s0074180900212746.

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Due to their high luminosity, the importance of understanding the massive star formation and evolution of giant Hii regions has become more and more evident in the last few years. A mayor scenario where giant H ii regions form and develop are the very inner parts of some galaxies. These bursts frequently are arranged in a ring-like pattern. We present a study of the stellar populations and gas physical conditions in circumnuclear star-forming regions (CNSFR) based on broad- and narrow-band photometry and spectrophotometric data, which have been analyzed with the use of evolutionary population synthesis and photo-ionization models. It is found that most CNSFRs show composite stellar populations of slightly different ages. They seem to have the highest abundances found in H ii region-like objects, showing also N/O overabundances and S/O underabundaces by a factor of about three. Also, CNSFRs as a class segregate from the disk H ii region family, clustering around higher ionizing temperatures.
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5

Kaltcheva, Nadia, Vincent Fabbri, Timothy Conard, and Valeri Golev. "Cepheus Star-Forming Field Revisited." International Journal of Astronomy and Astrophysics 03, no. 04 (2013): 472–79. http://dx.doi.org/10.4236/ijaa.2013.34054.

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6

Barthel, Peter. "Star-forming AGN host galaxies." New Astronomy Reviews 45, no. 9-10 (October 2001): 591–99. http://dx.doi.org/10.1016/s1387-6473(01)00139-7.

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7

Nisini, Brunella, and Teresa Giannini. "H2O in Star Forming Regions." Highlights of Astronomy 12 (2002): 67–69. http://dx.doi.org/10.1017/s1539299600012855.

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AbstractThis paper will review the importance of the water molecule in the various stages of the star formation process, addressing in particular how the recent observations obtained with the ISO and SWAS satellites have challenged the existing theoretical models.
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8

Bartkiewicz, Anna, and Huib Jan van Langevelde. "Masers in star forming regions." Proceedings of the International Astronomical Union 8, S287 (January 2012): 117–26. http://dx.doi.org/10.1017/s1743921312006771.

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AbstractMaser emission plays an important role as a tool in star formation studies. It is widely used for deriving kinematics, as well as the physical conditions of different structures, hidden in the dense environment very close to the young stars, for example associated with the onset of jets and outflows. We will summarize here the recent observational and theoretical progress on this topic since the last maser symposium: the IAU Symposium 242 in Alice Springs.
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9

Hodapp, Klaus-Werner, and John Rayner. "The S106 star-forming region." Astronomical Journal 102 (September 1991): 1108. http://dx.doi.org/10.1086/115937.

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10

Barthel, P. D. "Star-forming QSO host galaxies." Astronomy & Astrophysics 458, no. 1 (October 2006): 107–11. http://dx.doi.org/10.1051/0004-6361:20053591.

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11

Hasegawa, Tetsuo. "The Orion Star-Forming Complex." Symposium - International Astronomical Union 115 (1987): 123–37. http://dx.doi.org/10.1017/s0074180900095115.

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High resolution images of the Orion Nebula in the millimeter wave emission lines of CS and CO taken with the 45-m telescope at Nobeyama are presented. They cover a field approximately 400″ square with a 15″ – 34″ resolution and reveal a wealth of information on kinematic and density structures. The images of the J=1-0 (49 GHz) and J=2-1 (98 GHz) lines of CS show a long (>1 pc) and narrow (∼0.1 pc) N-S ridge of dense molecular gas. On the ridge, two major clumps are recognized; one is associated with the KL object and the other is 100″ south of it. The images of the J=1-0 (115 GHz) CO line indicate interaction between the molecular cloud and the H II region formed by the Trapezium stars. Bright CO emission is found towards the edges of the denser part of the H II region delineated by radio continuum emission. The CO emission coincides with the emission of vibrationally excited H2 and the 3.3 μm dust emission feature. The CO images reveal filamentary structures (“streamers”) stretching radially from the KL region. On the streamers there are Herbig-Haro objects moving away from the KL region. They may be tracers of weak interaction between the ambient molecular gas and mostly unseen, highly collimated, high-velocity (>200 km/s) jets.
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12

Cohen, R. J. "Masers in Star Forming Regions." Symposium - International Astronomical Union 115 (1987): 333–34. http://dx.doi.org/10.1017/s0074180900095711.

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OH and H2O masers in star forming regions are important because they are readily detectable indicators of star formation and because they provide unique information on the kinematics and physical conditions in high density regions (106 – 1010 cm−3) surrounding young stars, regions which cannot be studied by other means at present. The Jodrell Bank MERLIN interferometer has been used to map a sample of OH and H2O masers associated with bipolar molecular outflows. The maps of Cepheus A show that the masers are closely associated with the densest compact H II regions at the centre of the flow. The masers appear to be located at the inner edges of the circumstellar disk thought to play a role in collimating the outflow. It is suggested that the H2O masers trace the interaction between the stellar wind and the dense molecular gas, and the OH masers trace shocks propagating into the molecular gas. Rapid and sometimes correlated variations in the maser emission suggest that radiative pumping is likely in this source (Rowland and Cohen, Mon. Not. R. Astr. Soc. in press). Study of the other sources is still in progress.
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13

Tielens, A. G. G. M., and D. C. B. Whittet. "Ices in star forming regions." Symposium - International Astronomical Union 178 (1997): 45–60. http://dx.doi.org/10.1017/s0074180900009232.

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IR spectra of sources associated with molecular cloud material show a variety of absorption features attributed to simple molecules, such as H2O, CO, CH3OH, CO2, CH4, and OCS in icy grain mantles. These identifications are reviewed. These molecules are formed through accretion and reaction of gas phase species on grain surfaces. The high abundance of CH3OH and CO2 point towards the importance of hydrogenation and oxidation reactions in this process. Observations also show that thermal outgassing is of great importance for the composition of interstellar ice mantles. Both these processes are discussed in some detail.
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14

Ranalli, P. "The faintest star forming galaxies." Astronomische Nachrichten 324, no. 12 (February 2003): 143. http://dx.doi.org/10.1002/asna.200310042.

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15

Adams, Fred C., and David N. Spergel. "Lithopanspermia in Star-Forming Clusters." Astrobiology 5, no. 4 (August 2005): 497–514. http://dx.doi.org/10.1089/ast.2005.5.497.

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16

Ward, Rachel L., James Wadsley, and Alison Sills. "Unbound star-forming molecular clouds." Monthly Notices of the Royal Astronomical Society 439, no. 1 (January 30, 2014): 651–58. http://dx.doi.org/10.1093/mnras/stu004.

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17

Herbst, Eric. "Chemistry of Star-Forming Regions." Journal of Physical Chemistry A 109, no. 18 (May 2005): 4017–29. http://dx.doi.org/10.1021/jp050461c.

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18

Charnley, S. B. "Acetaldehyde in star-forming regions." Advances in Space Research 33, no. 1 (January 2004): 23–30. http://dx.doi.org/10.1016/j.asr.2003.08.005.

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19

Cohen, R. J. "Masers in star-forming regions." Astrophysics and Space Science 224, no. 1-2 (February 1995): 55–62. http://dx.doi.org/10.1007/bf00667821.

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20

Barro, Guillermo, S. M. Faber, David C. Koo, Avishai Dekel, Jerome J. Fang, Jonathan R. Trump, Pablo G. Pérez-González, et al. "Structural and Star-forming Relations sincez∼ 3: Connecting Compact Star-forming and Quiescent Galaxies." Astrophysical Journal 840, no. 1 (May 4, 2017): 47. http://dx.doi.org/10.3847/1538-4357/aa6b05.

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21

Chen, Zhengyi, Qiu-Sheng Gu, Rubén García-Benito, Zhi-Yu Zhang, Xue Ge, Mengyuan Xiao, and Xiaoling Yu. "PGC 38025: A Star-forming Lenticular Galaxy with an Off-nuclear Star-forming Core." Astrophysical Journal 915, no. 1 (June 28, 2021): 1. http://dx.doi.org/10.3847/1538-4357/abfb62.

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22

Taniguchi, Kotomi, Masao Saito, and Hiroyuki Ozeki. "13C ISOTOPIC FRACTIONATION OF HC3N IN STAR-FORMING REGIONS: LOW-MASS STAR-FORMING REGION L1527 AND HIGH-MASS STAR-FORMING REGION G28.28-0.36." Astrophysical Journal 830, no. 2 (October 17, 2016): 106. http://dx.doi.org/10.3847/0004-637x/830/2/106.

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23

Mihos, J. Christopher, and Lars Hernquist. "Star-forming galaxy models: Blending star formation into TREESPH." Astrophysical Journal 437 (December 1994): 611. http://dx.doi.org/10.1086/175025.

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24

Kainulainen, J., K. Lehtinen, P. Väisänen, L. Bronfman, and J. Knude. "A comparison of density structures of a star forming and a non-star-forming globule." Astronomy & Astrophysics 463, no. 3 (December 19, 2006): 1029–37. http://dx.doi.org/10.1051/0004-6361:20066431.

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25

Ballantyne, D. R., J. N. Armour, and J. Indergaard. "THE STAR FORMATION LAWS OF EDDINGTON-LIMITED STAR-FORMING DISKS." Astrophysical Journal 765, no. 2 (February 27, 2013): 138. http://dx.doi.org/10.1088/0004-637x/765/2/138.

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26

Duarte Puertas, S., J. M. Vilchez, J. Iglesias-Páramo, C. Kehrig, E. Pérez-Montero, and F. F. Rosales-Ortega. "Aperture-free star formation rate of SDSS star-forming galaxies." Astronomy & Astrophysics 599 (March 2017): A71. http://dx.doi.org/10.1051/0004-6361/201629044.

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27

Origlia, Livia, and Ernesto Oliva. "Red supergiants in star-forming galaxies." Symposium - International Astronomical Union 193 (1999): 613. http://dx.doi.org/10.1017/s007418090020644x.

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We present some results on the burst properties in star forming galaxies, using near infrared stellar features typical of red supergiants and Brackett nebular lines which trace the presence of luminous H II regions.
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28

Cerviño, Miguel, R. Diehl, K. Kretschmer, and S. Plüschke. "Radioactive isotopes in star forming regions." New Astronomy Reviews 46, no. 8-10 (July 2002): 541–45. http://dx.doi.org/10.1016/s1387-6473(02)00198-7.

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29

Gonidakis, I., E. Livanou, E. Kontizas, U. Klein, M. Kontizas, D. Kester, Y. Fukui, N. Mizuno, and P. Tsalmantza. "Star-Forming Regions in the SMC." Proceedings of the International Astronomical Union 2, S235 (August 2006): 311. http://dx.doi.org/10.1017/s1743921306006764.

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AbstractSMC has been going through an active star formation epoch, especially during the last 0.2 Gyr when the close encounter with the LMC occured. Our goal is to detect regions dominated by early-type stars and gas and examine their behaviour at different wavelengths. Spectral energy distributions, a colour-magnitude diagram and a two-colour diagram from IRAS data (Bontekoe, Koperet & Kester (1994); Bontekoe, Kester, Stanimirović, et al. (1999)) for these regions were used in order to compare their properties with those of starburst galaxies (Helou (1986); Lehnert & Heckman (1995)). We have selected 50 stellar complexes with increased 100-μm IRAS flux, with detetected emission in all IRAS bands and/or high concentration of young stars. Ranking them by size (Maragoudaki, Kontizas, Kontizas, et al. (1998)), a total of what we call 24 aggregates, 23 complexes and 3 super-complexes were found. Radio continuum maps at 8.6-GHz (Haynes, Murray, Klein, et al. (1986)) and the CO (1→0) line (Mizuno, Rubio, Mizuno, et al. (2001)) were also correlated with the map of the complexes. Only 8 of them show enhanced star formation activity according to their IR properties and 8.6-GHz map, however, none of them resembles the IR behaviour of starburst regions found in the LMC and starburst galaxies (Livanou, Kontizas, Gonidakis, et al. (2006)). The south-west part of the “bar” has the most diverse intensity of star formation, with CO emission coincident with the largest structure. In the north-eastern end of the “bar”, star formation is likely to have commenced in the recent past, with molecular gas being abundant in this region. Ongoing and future star formation are revealed in the wing, while it appears to have ceased in the central “bar”.
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30

Di Francesco, James. "Star-forming Substructure within Molecular Clouds." Proceedings of the International Astronomical Union 8, S292 (August 2012): 29–34. http://dx.doi.org/10.1017/s1743921313000185.

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AbstractWide-field far-infrared/submillimeter continuum maps of molecular clouds by the Herschel Space Observatory GBS and HOBYS surveys are revealing the star-forming substructures that lead to star formation in dense gas. In particular, these maps have revealed the central role in clouds of filaments, likely formed through turbulent motions. These filaments appear to be non-isothermal and fragment into cores only when their column densities exceed a stability threshold. Organizations of filament networks suggest the relative role of turbulence and gravity can be traced in different parts of a cloud, and filament intersections may lead to larger amounts of mass flow that form the precursors of high-mass stars or clusters.
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31

Henkel, C., J. G. Mangum, J. Darling, and K. M. Menten. "Densitometry of Active Star Forming Galaxies." Proceedings of the International Astronomical Union 8, S292 (August 2012): 239–42. http://dx.doi.org/10.1017/s1743921313001178.

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AbstractAttempting to distangle density and kinetic temperature of the star forming molecular gas in the central regions of galaxies, we have embarked on a project involving sensitive measurements of a variety of formaldehyde (H2CO) and ammonia (NH3) transitions. Preliminary results, based on observations from the Green Bank Telescope (GBT) and the Very Large Array (VLA) are summarized and an outline for the entire project is given.
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32

Xiao, Ting, Tinggui Wang, Huiyuan Wang, Hongyan Zhou, Honglin Lu, and Xiaobo Dong. "Dust reddening in star-forming galaxies." Proceedings of the International Astronomical Union 8, S292 (August 2012): 291. http://dx.doi.org/10.1017/s1743921313001452.

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AbstractDust is a crucial component of galaxies in modifying the observed properties of galaxies. Previous studies have suggested that dust reddening in star-forming galaxies is correlated with star formation rate (SFR), luminosity, gas-phase metallicity (Z), stellar mass (M*) and inclination. In this work we investigate the fundamental relations between dust reddening and physical properties of galaxies, and obtain a well-defined empirical recipe for dust reddening. The empirical formulae can be incorporated into semi-analytical models of galaxy formation and evolution to estimate the dust reddening and facilitate comparison with observations.
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33

van Dishoeck, Ewine F., and Geoffrey A. Blake. "CHEMICAL EVOLUTION OF STAR-FORMING REGIONS." Annual Review of Astronomy and Astrophysics 36, no. 1 (September 1998): 317–68. http://dx.doi.org/10.1146/annurev.astro.36.1.317.

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34

Kogure, Tomokazu. "The Star Forming Regions of Orion." International Astronomical Union Colloquium 148 (1995): 357–64. http://dx.doi.org/10.1017/s0252921100022181.

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AbstractThe distribution of emission line stars in Orion is presented, based on our recent surveys and other previous ones. Particular attention is given for the central 10 × 10 square degrees to compare some properties of emission line stars and OB association stars. As a result, a possibility of bimodal star formation is suggested in this region.
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35

Zezas, A. L., I. Georgantopoulos, and M. J. Ward. "X-ray luminous star-forming galaxies." Astronomical & Astrophysical Transactions 18, no. 3 (December 1999): 425–29. http://dx.doi.org/10.1080/10556799908202998.

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36

Gustafsson, Bengt. "Dust cleansing of star-forming gas." Astronomy & Astrophysics 616 (August 2018): A91. http://dx.doi.org/10.1051/0004-6361/201732354.

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Aims. We explore the possibility that solar chemical composition, as well as the similar composition of the rich open cluster M 67, have been affected by dust cleansing of the presolar or precluster cloud due to the radiative forces from bright early-type stars in its neighbourhood. Methods. We estimate possible cleansing effects using semi-analytical methods, which are essentially based on momentum conservation. Results. Our calculations indicate that the amounts of cleansed neutral gas are limited to a relatively thin shell surrounding the H II region around the early-type stars. Conclusions. It seems possible that the proposed mechanism acting in individual giant molecular clouds may produce significant abundance effects for masses corresponding to single stars or small groups of stars. The effects of cleansing are, however, severely constrained by the thinness of the cleansed shell of gas and by turbulence in the cloud. This is why the mechanism can hardly be important in cleansing masses corresponding to rich clusters, such as the mass of the original M 67.
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37

Gustafsson, Bengt. "Dust cleansing of star-forming gas." Astronomy & Astrophysics 620 (November 28, 2018): A53. http://dx.doi.org/10.1051/0004-6361/201833353.

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Aims. The possibility that the chemical composition of the solar atmosphere has been affected by radiative dust cleansing of late and weak accretion flows by the proto-sun itself is explored. Methods. Estimates, using semi-analytical methods and numerical simulations of the motion of dust grains in a collapsing non-magnetic and non-rotating gas sphere with a central light source are made in order to model possible dust-cleansing effects. Results. Our calculations indicate that the amount of cleansed material may well be consistent with the abundance differences observed for the Sun when compared with solar-like stars and with the relations found between these differences and the condensation temperature of the element. Conclusions. It seems quite possible that the proposed mechanism produced the significant abundance effects observed for the Sun, provided that late and relatively weak accretion did occur. The effects of cleansing may, however, be affected by outflows from the Sun, the existence and dynamics of magnetic fields and of the accretion disk, and the possible presence and location of the early Sun in a rich stellar cluster.
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38

Bayet, E., S. Viti, D. A. Williams, and J. M. C. Rawlings. "Emission from extragalactic star forming gas." EAS Publications Series 31 (2008): 165–67. http://dx.doi.org/10.1051/eas:0831032.

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39

Verma, R. P. "Cold Sources in Star Forming Regions." EAS Publications Series 4 (2002): 117. http://dx.doi.org/10.1051/eas:2002066.

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40

Maschberger, Th, C. J. Clarke, I. A. Bonnell, and P. Kroupa. "Properties of hierarchically forming star clusters." Monthly Notices of the Royal Astronomical Society 404, no. 2 (May 4, 2010): 1061–80. http://dx.doi.org/10.1111/j.1365-2966.2010.16346.x.

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41

Vijayan, Aditi, Biman B. Nath, Prateek Sharma, and Yuri Shchekinov. "Radio haloes of star-forming galaxies." Monthly Notices of the Royal Astronomical Society 492, no. 2 (December 23, 2019): 2924–35. http://dx.doi.org/10.1093/mnras/stz3568.

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ABSTRACT We study the synchrotron radio emission from extra-planar regions of star-forming galaxies. We use ideal magnetohydrodynamic simulations of a rotating Milky Way-type disc galaxy with distributed star formation sites for three star formation rates (0.3, 3, 30 M⊙ yr−1). From our simulations, we see emergence of galactic-scale magnetized outflows, carrying gas from the disc. We compare the morphology of the outflowing gas with hydrodynamic simulations. We look at the spatial distribution of magnetic field in the outflows. Assuming that a certain fraction of gas energy density is converted into cosmic ray energy density, and using information about the magnetic field, we obtain synchrotron emissivity throughout the simulation domain. We generate the surface brightness maps at 1.4 GHz. The outflows are more extended in the vertical direction than radial and hence have an oblate shape. We further find that the matter right behind the outer shock shines brighter in these maps than that above or below. To understand whether this feature can be observed, we produce vertical intensity profiles. We convolve the vertical intensity profile with the typical beam sizes of radio telescopes, for a galaxy located at 10 Mpc to estimate the radio scale height and compare with observations. The radio scale height is ∼300–1200 pc, depending on the resolution of the telescope. We relate the advection speed of the outer shock with the surface density of star formation as ${\rm v}_{\rm adv} \propto \Sigma _{\rm SFR}^{0.3}$, which is consistent with earlier observations and analytical estimates.
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42

Esteban, César. "Local high-mass star-forming regions." New Astronomy Reviews 44, no. 4-6 (July 2000): 205–12. http://dx.doi.org/10.1016/s1387-6473(00)00037-3.

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43

Forrest, W. J., and M. A. Shure. "Unipolar bubbles in star-forming regions." Astrophysical Journal 311 (December 1986): L81. http://dx.doi.org/10.1086/184802.

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44

Morata, O., R. Estalella, R. Lopez, and P. Planesas. "CS observations of star-forming regions." Monthly Notices of the Royal Astronomical Society 292, no. 1 (November 21, 1997): 120–32. http://dx.doi.org/10.1093/mnras/292.1.120.

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45

Schmeja, S., and R. S. Klessen. "Evolving structures of star-forming clusters." Astronomy & Astrophysics 449, no. 1 (March 16, 2006): 151–59. http://dx.doi.org/10.1051/0004-6361:20054464.

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46

Williams, David A., and Thomas W. Hartquist. "The Chemistry of Star-Forming Regions." Accounts of Chemical Research 32, no. 4 (April 1999): 334–41. http://dx.doi.org/10.1021/ar970114o.

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47

VAN LOO, S., S. A. E. G. FALLE, T. W. HARTQUIST, O. HAVNES, and G. E. MORFILL. "Dusty magnetohydrodynamics in star-forming regions." Journal of Plasma Physics 76, no. 3-4 (January 22, 2010): 569–78. http://dx.doi.org/10.1017/s0022377809990894.

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AbstractStar formation occurs in dark molecular regions where the number density of hydrogen nuclei nH exceeds 104 cm−3 and the fractional ionization is 10−7 or less. Dust grains with sizes ranging up to tenths of microns and perhaps down to tens of nanometers contain just less than 1% of the mass. Recombination on grains is important for the removal of gas-phase ions, which are produced by cosmic rays penetrating the dark regions. Collisions of neutrals with charged grains contribute significantly to the coupling of the magnetic field to the neutral gas. Consequently, the dynamics of the grains must be included in the magnetohydrodynamic models of large-scale collapse, the evolution of waves and the structures of shocks important in star formation.
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48

Mathieu, Robert D. "Stellar Kinematics in Star-Forming Regions." Symposium - International Astronomical Union 115 (1987): 61. http://dx.doi.org/10.1017/s0074180900094869.

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High-precision radial-velocity studies of four star-forming regions: λ Orionis, NGC 2264, the Trapezium cluster and Taurus-Auriga, are completed or in process (in collaboration with Latham, Marschall and Hartmann). Single-order (∼ 50 Å, central wavelength 5200 Å) echelle spectra have been obtained for late-type pre-main sequence stars. Measurement errors of 0.7 – 1.5 km/sec are typical, although some stars do not permit any radial-velocity measurement due to stellar rotation or spectral peculiarities.
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49

Gustavo, Bruzual A., and Magris C. Gladis. "Emission Lines in Star Forming Galaxies." Symposium - International Astronomical Union 164 (1995): 428. http://dx.doi.org/10.1017/s007418090010943x.

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Magris et al. (1993, Proceedings of the ESO/OHP Workshop on Dwarf Galaxies, ed. G. Meylan) have combined the spectral evolution population synthesis code of Bruzual & Charlot (1993, ApJ 405, 538) with the multipurpose photoionization-shock code MAPPINGS (Binette et al. 1993, AJ 105, 797) in order to calculate self-consistently the evolution of the nebular emission corresponding to the ionizing spectra produced by the synthetic population. In this poster we compare the redshift dependence of the EW[OII]3727 predicted by the Magris et al. models with the observations available (Colles et al. 1990, MNRAS 244, 408; Kennicutt 1992, ApJS 79, 255; Le Fevre et al. 1994, ApJ 423, L89). Models in which stars form following the Salpeter IMF according to the SFR Ψ(t) = 1M⊙τ−1exp(–t/τ), for τ = 1, 2, 3, 5, 7, and ∞ Gyr have been considered. We assume Ho = 50, Ω = 0, tg = 16 Gyr. About 2/3 of the galaxies in these samples have EW[OII]3727 from 2 to 5 times larger than the ones predicted by our models for steadily decreasing or even constant (τ = ∞) SFR. To cover the range of observed values of EW[OII]3727 we assume that instantaneous bursts (Salpeter IMF) of star formation take place in these galaxies, superimposed on the steady SFR used in the models. The mass added by the bursts as newly formed stars per unit mass of stars in the underlying galaxy is in the range 1 – 4 × 10−4. Depending on the rest-frame wavelength, the color of the galaxies may remain unaffected or become considerably bluer as a consequence of the bursting activity.
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50

Garrod, Robin T., Susanna L. Widicus Weaver, and Eric Herbst. "Complex chemistry in star-forming regions." Proceedings of the International Astronomical Union 4, S251 (February 2008): 123–24. http://dx.doi.org/10.1017/s1743921308021339.

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AbstractWe present a new gas-grain chemical model that allows the grain-surface formation of saturated, complex, organic species from their constituent functional-groups–basic building blocks that derive from the cosmic ray-induced photodissociation of the granular ice mantles. The surface mobility of the funtional-group radicals is crucial to the reactions, and much of the formation of complex molecules occurs at the intermediate temperatures (~20–40 K) attained during the warm-up of the hot core. Our model traces the evolution of a large range of detected, and as yet un-detected, complex molecules.
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