Relevant bibliographies by topics / Star forming region

Academic literature on the topic 'Star forming region'

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Published: 10 March 2023

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Journal articles on the topic "Star forming region"

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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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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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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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Dickel, H. R., W. M. Goss, and A. H. Rots. "Characteristics of H2CO Towards Star-Forming Regions." Symposium - International Astronomical Union 115 (1987): 171. http://dx.doi.org/10.1017/s0074180900095309.

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Small clusters of recently-formed massive stars with their associated compact H II regions are often found embedded in the dense cores of molecular clouds. The H2CO opacity is correlated with the compactness of the H II region and is especially high for those with associated maser activity although additional factors are involved for the ultra-compact H II regions (UCH II). VLA observations of H2CO at 2 cm have been made towards the UCH II regions of W49-north. The highest H2CO opacity of 1.0 is found towards region A which does not have maser activity; yet one of the most compact region C, has an H2CO opacity of only 0.3, For these sources the integrated H2CO opacity (over the entire profile) may be more indicative of compactness. This may be due to the broader H2CO lines which can occur towards the maser regions. For example, large line widths of 10 to 12 km s−1 ate found towards W49-north G where the most intense water masers are located and towards W49-north B which has OH masers. The H2CO line with the highest 2 cm opacity of 2.5 and a narrow width of 2 km s−1 is found towards the UCH II region ON 3 which has only weak H2O maser emission.
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Medina, N., J. Borissova, R. Kurtev, J. Alonso-García, Carlos G. Román-Zúñiga, A. Bayo, Marina Kounkel, et al. "The G 305 Star-forming Region. II. Irregular Variable Stars." Astrophysical Journal 914, no. 1 (June 1, 2021): 28. http://dx.doi.org/10.3847/1538-4357/abf639.

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Borissova, Jura, Alexandre Roman-Lopes, Kevin Covey, Nicolas Medina, Radostin Kurtev, Carlos Roman-Zuniga, M. A. Kuhn, et al. "The G305 Star-forming Region. I. Newly Classified Hot Stars." Astronomical Journal 158, no. 1 (July 8, 2019): 46. http://dx.doi.org/10.3847/1538-3881/ab276b.

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Daffern-Powell, Emma C., and Richard J. Parker. "Dynamical evolution of fractal structures in star-forming regions." Monthly Notices of the Royal Astronomical Society 493, no. 4 (February 28, 2020): 4925–35. http://dx.doi.org/10.1093/mnras/staa575.

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ABSTRACT The $\mathcal {Q}$-parameter is used extensively to quantify the spatial distributions of stars and gas in star-forming regions as well as older clusters and associations. It quantifies the amount of structure using the ratio of the average length of the minimum spanning tree, $\bar{m}$, to the average length within the complete graph, $\bar{s}$. The interpretation of the $\mathcal {Q}$-parameter often relies on comparing observed values of $\mathcal {Q}$, $\bar{m}$, and $\bar{s}$ to idealized synthetic geometries, where there is little or no match between the observed star-forming regions and the synthetic regions. We measure $\mathcal {Q}$, $\bar{m}$, and $\bar{s}$ over 10 Myr in N-body simulations, which are compared to IC 348, NGC 1333, and the ONC. For each star-forming region, we set up simulations that approximate their initial conditions for a combination of different virial ratios and fractal dimensions. We find that the dynamical evolution of idealized fractal geometries can account for the observed $\mathcal {Q}$, $\bar{m}$, and $\bar{s}$ values in nearby star-forming regions. In general, an initially fractal star-forming region will tend to evolve to become more smooth and centrally concentrated. However, we show that different initial conditions, as well as where the edge of the region is defined, can cause significant differences in the path that a star-forming region takes across the $\bar{m}{-}\bar{s}$ plot as it evolves. We caution that the observed $\mathcal {Q}$-parameter should not be directly compared to idealized geometries. Instead, it should be used to determine the degree to which a star-forming region is either spatially substructured or smooth and centrally concentrated.
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Yamamoto, Satoshi, Hitomi Mikami, and Shuji Saito. "SiO in Star Forming Regions: Barnard 1 and Orion KL." International Astronomical Union Colloquium 140 (1994): 243–44. http://dx.doi.org/10.1017/s0252921100019618.

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AbstractInterferometric observations of the SiO (J = 2 − 1) line are carried out toward a low-mass-star forming region, Bl, and a massive star forming region, Ori KL. Production mechanisms of SiO in these regions are discussed.
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Bian, S. B., Y. Xu, J. J. Li, Y. W. Wu, B. Zhang, X. Chen, Y. J. Li, Z. H. Lin, C. J. Hao, and D. J. Liu. "Parallax of Star-forming Region G027.22+0.14." Astronomical Journal 163, no. 2 (January 11, 2022): 54. http://dx.doi.org/10.3847/1538-3881/ac3d90.

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Abstract Using the Very Long Baseline Array, we measured the trigonometric parallax and proper motions toward a 6.7 GHz methanol maser in the distant high-mass star-forming region G027.22+0.14. The distance of this source is determined to be 6.3 − 0.5 + 0.6 kpc. Combining its Galactic coordinates, radial velocity, and proper motion, we assign G027.22+0.14 to the far portion of the Norma arm. The low peculiar motion and lower luminosity of G027.22+0.14 support the conjecture by Immer et al. that low-luminosity sources tend to have low peculiar motions.
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Walsh, A. J., J. K. Lee, and M. G. Burton. "The massive star forming region G323.74−0.26." Monthly Notices of the Royal Astronomical Society 329, no. 2 (January 2002): 475–80. http://dx.doi.org/10.1046/j.1365-8711.2002.05006.x.

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Dissertations / Theses on the topic "Star forming region"

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Revelle, Melissa C. "OBSERVATIONS OF STAR FORMING REGION NGC 1333." Thesis, The University of Arizona, 2009. http://hdl.handle.net/10150/192971.

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Rane, Akshaya. "Physical Conditions in a Galactic Star forming region W22." UKnowledge, 2011. http://uknowledge.uky.edu/gradschool_theses/158.

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This document describes study of an active star forming region in our galaxy (the Milky Way) known as W22. Physical conditions in these regions can help us in understanding star formation processes in the universe and hence the structure and evolution of the universe. Zeeman effect measurements in 18 cm OH absorption line were carried out in order to estimate the line of sight magnetic field strength in the molecular cloud associated with this star forming region. Other physical parameters such as hydrogen column density, optical depth, critical magnetic field were also determined from these measurements. The region was mapped at 18 cm and the distribution of molecular gas within this star forming complex was described.
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Verdirame, Chiara. "The core mass function in star-forming region NGC6357." Master's thesis, Alma Mater Studiorum - Università di Bologna, 2014. http://amslaurea.unibo.it/6581/.

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The aim of this work was to study the dense cloud structures and to obtain the mass distribution of the dense cores (CMF) within the NGC6357 complex, from observations of the dust continuum at 450 and 850~$\mu$m of a 30 $\times$ 30 arcmin$^2$ region containing the H\textsc{ii} regions, G353.2+0.9 and G353.1+0.6.
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Buenzli, Esther. "Observation, modeling and interpretation of the star forming region S140." Zürich : ETH, Eidgenössische Technische Hochschule Zürich, Institute of Astronomy, 2007. http://e-collection.ethbib.ethz.ch/show?type=dipl&nr=298.

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Garden, Rognvald Peebles. "An infrared and millimeter-wave spectroscopic study of the DR21 outflow." Thesis, University of Edinburgh, 1987. http://hdl.handle.net/1842/28084.

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In this thesis, new high-angular resolution infrared and millimeter-wave spectroscopic observations of the enigmatic outflow activity associated with the luminous DR21 star-form ing region are presented and discussed. The intent is to use these observations to undertake a detailed investigation of the physical nature of the central driving engine and the related dynamical processes involved in collimating the hypersonic outflow gas. In the infrared, large-scale mapping and high-spectral resolution profile measurements of the vibrational H2 v = l-0 S(l) line are used to investigate the morphology and kinematic structure of the hot, dense gas that is collisionally excited behind fast shocks. The H2 emission delineates a highly-collimated pair of bipolar jets that extend over a projected distance of ~ 5 pc, centred on the DR21 molecular cloud core; this is undoubtedly the most luminous (in H2 line emission) and extended galactic outflow source yet discovered. Furthermore, the H2 line profiles at certain locations within the jets possess high-velocity wings that extend to beyond 100 km s-1 from the DR21 rest velocity. These observations pose interesting dynamical consequencies as at such high velocities H 2 should be entirely dissociated. In an attempt to derive the mass distribution and velocity structure of the molecular gas participating in the outflow, and hence the driving force and associated mechanical luminosity, detailed observations were also undertaken at millimeter-wavelengths in the CO J= 1 -0 and CS J = l-0 , J= 2-l lines. It is found that the DR21 outflow is considerably more massive and energetic than any other outflow source studied to date. Another feature unique to the DR21 region is the discovery of extended high-velocity CS emission that is dynamically associated with the outflow lobes and extends to a distance of ~ 3 pc from the cloud core; this component presumably originates from am bient gas that has been swept up and compressed by the outflow. The high-velocity CS may be overabundant by 2 orders of magnitude, in good agreement with current numerical models of post-shock chemistry. The CS observations further reveal the existence of an extremely massive, slowly rotating disc of high-density neutral gas that surrounds the central outflow source. It is most probable that the large momentum flux in outflow material derives from efficient mass-loss from the surface of this disc, mediated via a centrifugally propelled, magneto-hydrodynamic wind. An additional confinment mechanism is required to collimate the outflow at large distances from the flow origin. If this confinment is primarily pressure driven, then sudden changes in the ambient cloud pressure could induce a succession of oblique shocks within the outflow that may give rise to the periodic clumpy structure that characterizes the H2 emission-line jets. Other consequencies of the pressure-confinment mechanism are discussed and a broad resemblance to extragalactic radio jets is remarked upon.
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Dobson, Amy. "Kinematics and age spreads of the young star-forming region NGC 2264." Thesis, Keele University, 2016. http://eprints.keele.ac.uk/2413/.

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While stars are relatively well understood, the timescales on which they form are still debated. The young cluster NGC 2264 is an ideal region in which to test hypotheses about the timescale of star and cluster formation. Co-eval stars at any given e�ective temperature are expected to have similar luminosities and radii, but previous research on clusters, including NGC 2264, has found that this may not be the case. In this thesis, �bre spectroscopy from the FLAMES spectrograph is used to �nd radial and projected equatorial velocities for many low-mass pre-main sequence stars in NGC 2264. Projected radii are estimated by combining these data with published rotation periods. The projected radius distribution is compared with models incorporating radius and age dispersions. These methods circumvent many uncertainties that arise when using luminosities to infer ages from the Hertzsprung-Russell diagram (HRD). Comparisons of models and data favour a spread of radii that is inconsistent with a coeval population but consistent with the spread of ages seen in the HRD. Modeldependent, but distance-independent, ages of 1 - 2.6 Myrs are found, and agreement with ages determined from the HRD is found for a cluster distance of 770� 46 pc. The cluster velocity dispersion is well resolved, and a connection between spatial and kinematic substructure is established. The substructure is unlikely to be responsible for the observed age dispersion. A catalogue of 547 spectroscopic observations of stars in NGC 2264 is presented, with measurements of radial and projected equatorial velocities.
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Kovács, Gábor. "Infrared variability studies of low-mass stars in the field and in the Carina Nebula star forming region." Thesis, University of Cambridge, 2015. https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.709097.

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Czanik, Robert Johann. "An optical study of the high mass star forming region RCW 34 / Robert Johann Czanik." Thesis, North-West University, 2013. http://hdl.handle.net/10394/9102.

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This study consisted of an optical photometric and spectroscopic analysis on a 7′ 7′ field around the Southern high mass star forming region RCW 34. A previous study on RCW 34 in the NIR discov- ered many deeply embedded young stellar objects which were suspected to be T Tauri stars and which justified further investigation. The data used in this study consisted of three sets, the first two are photometric and spectroscopic data sets which were obtained during the first two weeks of February 2002. A third data set of spectroscopic observations was obtained by the author during the second week of 2011 of selected candidates using results from the NIR study and from the photometric data sets. All of the spectroscopy was conducted with the long slit spectrograph on the 1.9-m telescope and the photometry with DANDICAM on the 1.0-m telescope at the South African Astronomical Observatory (SAAO) in Sutherland. Objectives accomplished in the course of this study were to understand, ob- tain, reduce and interpret photometric and long slit spectroscopic CCD images. From the photometric results 57 stars showed excess blue emission on a colour-colour diagram which could be generated by circumstellar matter. The spectroscopic study showed 5 stars that showed H emission and 2 with strong Li absorption lines which confirm the suspicions of the NIR study about T Tauri stars in the region. All of the stars from the spectroscopic study in 2011 were identified as low-mass K or M type stars. Using colour-magnitude diagrams it was possible to see that the majority of the stars in the cluster are low-mass pre-main sequence stars. The stars matching between the optical and NIR filters were plotted on NIR colour-colour diagrams showing that the 5 stars that had H emission lines also had NIR colours characteristic to T Tauri stars. Out of the 5 stars that showed H emission, 2 were found to be classical T Tauris and three were found to be weak line T Tauris.
Thesis (MSc (Space Physics))--North-West University, Potchefstroom Campus, 2013
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Oskinova, L., R. Gruendl, Richard Ignace, Y. H. Chu, W. R. Hamann, and A. Feldmeier. "Hard X-ray Emission from the Massive Star-Forming Region ON 2: Discovery with XMM-Newton." Digital Commons @ East Tennessee State University, 2010. https://dc.etsu.edu/etsu-works/6259.

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We obtained X-ray XMM-Newton observations of the open cluster Berkeley 87 and the massive star-forming region (SFR) ON 2. In addition, archival infrared Spitzer Space Telescope observations were used to study the morphology of ON 2, to uncover young stellar objects, and to investigate their relationship with the X-ray sources. It is likely that the SFR ON 2 and Berkeley 87 are at the same distance, 1.23 kpc, and hence are associated. The XMM-Newton observations detected X-rays from massive stars in Berkeley 87 as well as diffuse emission from the SFR ON 2. The two patches of diffuse X-ray emission are encompassed in the shell-like H II region GAL 75.84+0.40 in the northern part of ON 2 and in the ON 2S region in the southern part of ON 2. The diffuse emission from GAL 75.84+0.40 suffers an absorption column equivalent to AV ≈ 28 mag. Its spectrum can be fitted either with a thermal plasma model at T ≳ 30 MK or by an absorbed power-law model with γ ≈ −2.6. The X-ray luminosity of GAL 75.84+0.40 is LX ≈ 6 × 1031 erg s−1. The diffuse emission from ON 2S is adjacent to the ultra-compact H II (UCH II) region Cygnus 2N, but does not coincide with it or with any other known UCH II region. It has a luminosity of LX ≈ 4 × 1031 erg s−1. The spectrum can be fitted with an absorbed power-law model with γ ≈ −1.4. We adopt the view of Turner & Forbes that the SFR ON 2 is physically associated with the massive star cluster Berkeley 87 hosting the WO-type star WR 142. We discuss different explanations for the apparently diffuse X-ray emission in these SFRs. These include synchrotron radiation, invoked by the co-existence of strongly shocked stellar winds and turbulent magnetic fields in the star-forming complex, cluster wind emission, or an unresolved population of discrete sources.
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Harayama, Yohei. "The IMF of the massive star-forming region NGC 3603 from NIR adaptive optics observations." Diss., [S.l.] : [s.n.], 2007. http://edoc.ub.uni-muenchen.de/archive/00007108.

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Books on the topic "Star forming region"

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Peimbert, Manuel, and Jun Jugaku, eds. Star Forming Regions. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5.

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Bo, Reipurth, and Astronomical Society of the Pacific., eds. Handbook of star forming regions. San Francisco: Astronomical Society of the Pacific, 2008.

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Bo, Reipurth, and Astronomical Society of the Pacific., eds. Handbook of star forming regions. San Francisco: Astronomical Society of the Pacific, 2008.

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F, Sterzik Michael, and United States. National Aeronautics and Space Administration., eds. Do star forming regions have different binary fractions? Garching, Germany: Max-Planck-Institut für Extraterrestrische Physik, 1995.

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F, Sterzik Michael, and United States. National Aeronautics and Space Administration., eds. Do star forming regions have different binary fractions? Garching, Germany: Max-Planck-Institut für Extraterrestrische Physik, 1995.

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HARTQUIST, T. W., J. M. PITTARD, and S. A. E. G. FALLE, eds. Diffuse Matter from Star Forming Regions to Active Galaxies. Dordrecht: Springer Netherlands, 2007. http://dx.doi.org/10.1007/978-1-4020-5425-9.

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Olofsson, Kjell. Spectral evolutionary synthesis models of metal-poor star forming regions. Uppsala: Uppsala Astronomical Observatory, 1988.

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1941-, Peimbert Manuel, and Jugaku Jun 1927-, eds. Star forming regions: Proceedings of the 115th Symposium of the International Astronomical Union held in Tokyo, Japan, November 11-15, 1985. Dordrecht: D. Reidel Pub. Co., 1987.

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United States. National Aeronautics and Space Administration., ed. The circumstellar environment of low mass star forming regions: Final technical report : Airborne Astronomy Program (NRA2-36449 (BXM)), grant NAG 2-959. [Washington, DC: National Aeronautics and Space Administration, 1997.

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Koenig, Xavier Paul. Star formation in W5: A Spitzer Survey of a massive star forming region. 2010.

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Book chapters on the topic "Star forming region"

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Walsh, J. R. "The Structure of the HH39 Region." In Star Forming Regions, 340–41. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_100.

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Moriguchi, H., and Y. Fukui. "CO Molecular Clouds in the Region of GL490." In Star Forming Regions, 358–59. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_109.

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Peimbert, M., M. Peña, and S. Torres-Peimbert. "NGC 2363, A Giant Extragalactic H II Region." In Star Forming Regions, 635–36. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_190.

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Hirabayashi, Hisashi, Kenji Akabane, Masaki Morimoto, Yosiaki Sofue, Makato Inoue, and Toshihiro Handa. "The Sgr B2 Region Seen at 43 GHz." In Star Forming Regions, 158–60. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_50.

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Massi, M., M. Felli, M. Catarzi, and M. Simon. "MON R2: A Blister Type H II Region." In Star Forming Regions, 193. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_72.

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Kuiper, T. B. H., W. L. Peters, F. F. Gardner, and J. B. Whiteoak. "The Star Forming Region in Bok Globule 210-6a." In Star Forming Regions, 364–65. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_113.

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Tapia, M., M. Roth, L. F. Rodríguez, J. Cantó, P. Persi, M. Ferrari-Toniolo, and J. A. López. "The Star Formation Region Associated with the Cometary Nebula GM24." In Star Forming Regions, 188. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_68.

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Vrba, F. J., R. Baierlein, and W. Herbst. "The Magnetic Field Structure of the CMa R1 Star Formation Region." In Star Forming Regions, 85–86. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_29.

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Persi, P., M. Ferrari-Toniolo, M. Roth, and M. Tapia. "Near-Infrared Sources in the Complex H II Region NGC 6357." In Star Forming Regions, 187–88. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_67.

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Garden, Rognvald P. "An Extremely Luminous H2 Flow in the DR21 Star Forming Region." In Star Forming Regions, 325–28. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_92.

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Conference papers on the topic "Star forming region"

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Das, Ankan, Sandip K. Chakrabarti, Kinsuk Acharyya, and Sonali Chakrabarti. "Methanol formation around the star forming region." In FIRST INTERNATIONAL CONFERENCE ON CHEMICAL EVOLUTION OF STAR FORMING REGION AND ORIGIN OF LIFE: Astrochem2012. AIP, 2013. http://dx.doi.org/10.1063/1.4812616.

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Wang, Zhong. "Measuring Star Forming Activities in The Antennae: Region-by-region." In THE SPECTRAL ENERGY DISTRIBUTIONS OF GAS-RICH GALAXIES: Confronting Models with Data; International Workshop. AIP, 2005. http://dx.doi.org/10.1063/1.1913961.

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Saha, Rajdeep, Liton Majumdar, Ankan Das, Sandip K. Chakrabarti, and Sonali Chakrabarti. "Formation of the nucleobases around the star forming region." In FIRST INTERNATIONAL CONFERENCE ON CHEMICAL EVOLUTION OF STAR FORMING REGION AND ORIGIN OF LIFE: Astrochem2012. AIP, 2013. http://dx.doi.org/10.1063/1.4812620.

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Imai, Hiroshi, Huib Jan van Langevelde, and Tomofumi Umemoto. "Water masers in the star forming region in L1287." In 8th European VLBI Network Symposium. Trieste, Italy: Sissa Medialab, 2007. http://dx.doi.org/10.22323/1.036.0076.

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Datta, Srabani. "Multiwavelength study of Barnard 1: A young star-forming region." In From Planets to Dark Energy: the Modern Radio Universe. Trieste, Italy: Sissa Medialab, 2008. http://dx.doi.org/10.22323/1.052.0088.

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Burgess, A., J. Bouvier, E. Moraux, and Eric Stempels. "Methane T-Dwarf Candidates in the Star Forming Region IC 348." In COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099159.

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Rawlings, J. M. C., N. J. Evans, and S. Zhou. "Models of molecular processes in the low mass star-forming region B335." In The 50th international meeting of physical chemistry: Molecules and grains in space. AIP, 1994. http://dx.doi.org/10.1063/1.46598.

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Petrashkevich, I. V., and A. F. Punanova. "Deuterium fraction in cold dense cores in the star-forming region L1688." In Всероссийская с международным участием научная конференция студентов и молодых ученых, посвященная памяти Полины Евгеньевны Захаровой «Астрономия и исследование космического пространства». Ural University Press, 2021. http://dx.doi.org/10.15826/b978-5-7996-3229-8.13.

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Abstract:
The work presents a study of deuterium fraction in cold dense cores in the low mass starforming region L1688. To study the deuterium fraction and its correlation with physical conditions in a cold dense core, we produced the observational maps of three pairs of species (N2H+ and N2D+, NH3 and NH2D, H13CO+ and DCO+) towards four cold dense cores. The observations were carried out with the IRAM 30m telescope (except for NH3 data taken from the GAS survey based on observations with GBT).
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9

Thompson, Will, Dariusz Lis, and Susanna Widicus Weaver. "NOEMA OBSERVATIONS OF COMPLEX ORGANIC CHEMISTRY IN THE W3 STAR-FORMING REGION." In 2022 International Symposium on Molecular Spectroscopy. Urbana, Illinois: University of Illinois at Urbana-Champaign, 2022. http://dx.doi.org/10.15278/isms.2022.mn01.

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10

Brunthaler, Andreas, Kazi Rygl, Karl M. Menten, Mark J. Reid, Huib Jan van Langevelde, Mareki Honma, Karl J. E. Torstensson, Kenta Fujisawa, and Alberto Sanna. "A preliminary distance to W75N in the Cygnus X star-forming region." In 10th European VLBI Network Symposium and EVN Users Meeting: VLBI and the new generation of radio arrays. Trieste, Italy: Sissa Medialab, 2011. http://dx.doi.org/10.22323/1.125.0103.

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Reports on the topic "Star forming region"

1

O'Shea, Brian. Forming a Primordial Star in a Relic HII Region. Office of Scientific and Technical Information (OSTI), April 2005. http://dx.doi.org/10.2172/839853.

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