Relevant bibliographies by topics / Star-forming

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  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers
  6. Reports

Academic literature on the topic 'Star-forming'

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

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Journal articles on the topic "Star-forming"

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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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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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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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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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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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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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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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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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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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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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Dissertations / Theses on the topic "Star-forming"

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Lee, Pawel. "Structure in star forming regions." Thesis, University of Sheffield, 2016. http://etheses.whiterose.ac.uk/12395/.

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Stars form in clumpy, highly substructured environments. In this thesis I set up N-body simulations of substructured star forming regions and investigate the impact that the substructure has on the survival of the star forming regions. I also present a broad range of methods used in other fields to quantify and identify structure. I discuss their strengths and shortcomings and assess their suitability for use in astronomical contexts. I use the Q and Λ methods to compare the distributions of class I and class II sources in observed star forming regions to learn more about the dynamical evolution of systems and infer whether they are bound or unbound.
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Gledhill, Timothy Michael. "Optical polarimetry of star forming regions." Thesis, Durham University, 1987. http://etheses.dur.ac.uk/6757/.

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Holdship, J. R. "Shock chemistry in star forming environments." Thesis, University College London (University of London), 2017. http://discovery.ucl.ac.uk/10027644/.

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Molecules are abundant in many astrophysical environments. The observation of these molecules and the modelling of the chemistry that leads to their formation is a powerful tool for improving our understanding of the regions in which they are found. In this thesis, a chemical model is developed and applied to astrophysical shocks to understand a number of processes in star forming regions. Shocks often result in discontinuous changes in the temperature and density of the gases they affect. The turbulent fragmentation theory of star formation suggests that such shocks are responsible for the over-densities that lead to the formation and collapse of prestellar cores from molecular clouds. Focusing on low mass objects, a chemical model of prestellar cores formed through shocks is developed and compared to models of similarly dense gas formed through gravitational freefall. Observational predictions of shock induced differences in the chemistry of these cores are reported and compared to the literature. Not only are molecules abundant in the gas phase but they are also observed in solid state, frozen onto the surfaces of interstellar dust grains. This freeze out process is efficient in molecular clouds but the composition of these ices is poorly constrained for all but the most abundant molecules. Shocks represent a powerful tool to study these ices as they not only change the gas properties but can also sputter and shatter dust grains releasing frozen molecules into the gas phase. Observations of sulfur-bearing molecules in a protostellar outflow, L1157-B1, are presented and analysed, giving an overview of the sulfur content of the recently shocked gas. The abundances of important sulfur molecules are then compared to chemical models of C-type shocks in an attempt to constrain the main solid state form of sulfur before the shock and the shock properties of the observed outflow.
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Lacki, Brian Cameron. "Cosmic Rays in Star-Forming Galaxies." The Ohio State University, 2011. http://rave.ohiolink.edu/etdc/view?acc_num=osu1313437011.

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Kalari, Venu Madhav. "Disc-accretion in star-forming regions." Thesis, Queen's University Belfast, 2015. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.695381.

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In this thesis, I present new ultraviolet/optical/infrared photometric and spectroscopic observations of pre-main sequence stars (PMS) that have formed either in metal-poor conditions, or in the vicinity of strong ionising radiation. This includes observations of 235 Classical T Tauri stars in the Lagoon Nebula; 63 Classical T Tauril Herbig Ae stars in the Carina Nebula open cluster Trumpler 14; 24 intermediate mass T Tauri stars in the low-Z Sh 2-284 star-forming region; and one Herbig 8[e] PMS candidate in the metal-poor 30 Doradus region. I measure the accretion rates of these PMS stars using the intensities of the U/Halpha band excess measured through either optical spectra of imaging. Where possible, I use archive infrared photometry in the 1.2-8 micron wavelength range to estimate the PMS disc evolutionary stage. The influence of the surrounding environment on the accretion rate evolution of pre-main sequence stars in these regions is explored using the spatial, and temporal distributions of accretion rate, mass, age and disc stage of PMS stars. In the wide-field photometric data of the Lagoon Nebula, I find that the spatial distributions of PMS stars is a continuum, ranging from dense clustering to relative isolation. Strongly accretion PMS stars are generally clumped together, in close proximity to their natal molecular cloud, whereas weaker, older accretors are relatively space apart. Ionising radiation from early-type stars appears to positively affect accretion rates on scales of 2-3 pc, but no evidence for triggered star formation is found. In addition, the accretion rates measured from Halpha imaging correlate well to those estimated from U-band photometry. In wide-field photometric data of Trumpler 14, I discover a population of PMS candidates nearly 25 Myrs old. I argue that these PMS candidates are a foreground population, approximately 5 Myr old that belong to the Carina Nebula cluster Trumpler 16. Using Halpha spectra of 24 intermediate mass T Tauri stars in Sh 2-284 (Z-0.004), I demonstrate that there is little evidence for a systematic change in accretion rates with metallicity, contrary to previous literature results at Z-0.006-0.002 in the Magellanic Clouds. I suggest that previous studies are likely affected by detection limits and biases. I also present ultraviolet/optical spectra of the Herbig 8[e] PMS candidate VFTS 822 located in the 30 Doradus region of the Large Magellanic Cloud. I discuss the impact of the discovery of VFTS 822 for star formation studies in the Magellanic Clouds, external Galaxies .
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Contreras, Peña Carlos Eduardo. "Exteme variables in star forming regions." Thesis, University of Hertfordshire, 2015. http://hdl.handle.net/2299/15590.

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The notion that low- to intermediate-mass young stellar objects (YSOs) gain mass at a constant rate during the early stages of their evolution appears to be challenged by observations of YSOs suffering sudden increases of the rate at which they gain mass from their circumstellar discs. Also, this idea that stars spend most of their lifetime with a low accretion rate and gain most of their final mass during short-lived episodes of high accretion bursts, helps to solve some long-standing problems in stellar evolution. The original classification of eruptive variables divides them in two separate subclasses known as FU Orionis stars (FUors) and EX Lupi stars (EXors). In this classical view FUors are at an early evolutionary stage and are still gaining mass from their parent envelopes, whilst EXors are thought to be older objects only surrounded by an accretion disc. The problem with this classical view is that it excludes younger protostars which have higher accretion rates but are too deeply embedded in circumstellar matter to be observed at optical wavelengths. Optically invisible protostars have been observed to display large variability in the near-infrared. These and some recent discoveries of new eruptive variables, show characteristics that can be attributed to both of the optically-defined subclasses of eruptive variables. The new objects have been proposed to be part of a new class of eruptive variables. However, a more accepted scenario is that in fact the original classes only represent two extremes of the same phenomena. In this sense eruptive variability could be explained as arising from one physical mechanism, i.e. unsteady accretion, where a variation in the parameters of such mechanism can cause the different characteristics observed in the members of this class. With the aim of studying the incidence of episodic accretion among young stellar objects, and to characterize the nature of these eruptive variables we searched for high amplitude variability in two multi-epoch infrared surveys: the UKIDSS Galactic Plane Survey (GPS) and the Vista Variables in the Via Lactea (VVV). In order to further investigate the nature of the selected variable stars, we use photometric information arising from public surveys at near- to farinfrared wavelengths. In addition we have performed spectroscopic and photometric follow-up for a large subset of the samples arising from GPS and VVV. We analyse the widely separated two-epoch K-band photometry in the 5th, 7th and 8th data releases of the UKIDSS Galactic Plane Survey. We find 71 stars with _K > 1 mag, including 2 previously known OH/IR stars and a Nova. Even though the mid-plane is mostly excluded from the dataset, we find the majority (66%) of our sample to be within known star forming regions (SFRs), with two large concentrations in the Serpens OB2 association (11 stars) and the Cygnus-X complex (27 stars). The analysis of the multi-epoch K-band photometry of 2010-2012 data from VVV covering the Galactic disc at |b| < 1◦ yields 816 high amplitude variables, which include known variables of different classes such as high mass X-ray binaries, Novae and eclipsing binaries among others. Remarkably, 65% of the sample are found concentrated towards areas of star formation, similar to the results from GPS. In both surveys, sources in SFRs show spectral energy distributions (SEDs) that support classification as YSOs. This indicates that YSOs dominate the Galactic population of high amplitude infrared variable stars at low luminosities and therefore likely dominate the total high amplitude population. Spectroscopic follow-up allows us to confirm the pre-main sequence nature of several GPS and VVV Objects. Most objects in both samples show spectroscopic signatures that can be attributed to YSOs undergoing high states of accretion, such as veiling of photospheric features and CO emission, or show FUor-like spectra. We also find a large fraction of objects with 2.12 μm H2 emission that can be explained as arising from shock-excited emission caused by molecular outflows. Whether these molecular outflows are related to outbursts events cannot be confirmed from our data. Adding the GPS and VVV spectroscopic results, we find that between 6 and 14 objects are new additions to the FUor class from their close resemblance to the near-infrared spectra of FUors, and at least 23 more objects are new additions to the eruptive variable class. For most of these we are unable to classify them into any of the original definitions for this variable class. In any case, we are adding up to 37 new stars to the eruptive variable class which would double the current number of known objects. We note that most objects are found to be deeply embedded optically invisible stars, thus increasing the number of objects belonging to this subclass by a much larger factor. In general, objects in our samples which are found to be likely eruptive variable stars show a mixture of characteristics that can be attributed to both of the optically-defined classes. This agrees well with the recent discoveries in the literature. Finally, we are able to derive a first rough estimate on the incidence of episodic accretion among class I YSOs in the star-forming complex G305. We find that _ 9% of such objects are in a state of high accretion. This number is in agreement with previous theoretical and observational estimates among class I YSOs.
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Mineo, Stefano. "X-ray emission from star-forming galaxies." Diss., lmu, 2011. http://nbn-resolving.de/urn:nbn:de:bvb:19-134839.

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Maskoliūnas, Marius. "Investigation of star forming regions in Cepheus." Doctoral thesis, Lithuanian Academic Libraries Network (LABT), 2014. http://vddb.library.lt/obj/LT-eLABa-0001:E.02~2014~D_20140203_133341-51153.

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The interstellar matter in the Galaxy is concentrated in a thin layer close to the galactic plane, mostly in spiral arms. Most of the interstellar matter is in a form of atomic and molecular gas and only 1% of its mass is in a form of small (0.01 – 0.1 µm) dust grains which absorb and scatter the light of stars and cause the interstellar extinction. A part of interstellar gas and dust are in a diffuse form and fill the space with density which exponentially decreases with the distance from the galactic plane. However, in the spiral arms gigantic molecular clouds are present which play an outstanding role in the evolution of the Galaxy, since in them star forming processes take place. Molecular and dust clouds, young star clusters and associations and other star forming regions are concentrated in the Milky Way plane. However, due to gravitational and radiation interactions between the molecular clouds and the young massive stars, some fragments of spiral arms deviate from the galactic plane. One of such deviating branches from the Local (Orion) spiral arm is a huge elongated system of molecular and dust clouds located in the Cepheus constellation which is known as the Cepheus Flare. Most of the objects investigated in this dissertation belong to this branch of the Local spiral arm. The objects selected for the investigation are star forming regions in the vicinity of the reflection nebula NGC 7023, a group of dark clouds TGU 619, the young open cluster NGC 7129 and the... [to full text]
Paukščių tako Galaktikoje didžioji dalis tarpžvaigždinės medžiagos yra susitelkusi į ploną sluoksnį Galaktikos plokštumoje, daugiausiai spiralinėse vijose. Didžiąją dalį tarpžvaigždinės medžiagos sudaro atominės ir molekulinės dujos ir tik maždaug 1% masės yra mažos (0.01 – 0.1 µm) dydžio dulkelės, kurios sugeria ir išsklaido šviesą ir sukelia tarpžvaigždinės ekstinkcijos reiškinį. Spiralinėse vijose esantys molekuliniai debesys yra svarbūs Galaktikos evoliucijos procese, nes juose vyksta aktyvūs žvaigždžių formavimosi procesai. Molekuliniai ir dulkių debesys, jaunų žvaigždžių spiečiai ir asociacijos bei kitos žvaigždžių susidarymo sritys dažniausiai yra Galaktikos plokštumoje. Tačiau dėl gravitacinės ir radiacinės sąveikos tarp jaunų didelės masės žvaigždžių ir molekulinių debesų kai kuriose Paukščių Tako srityse žvaigždėdaros rajonai nukrypsta nuo Galaktikos plokštumos. Viename iš tokių rajonų Cefėjo žvaigždyno kryptimi dalis tarpžvaigždinių debesų ir žvaigždėdaros rajonų yra nukrypę nuo Galaktikos plokštumos link šiaurinio dangaus poliaus ir sudaro Paukščių Tako atšaką, literatūroje žinomą kaip Cepheus Flare. Dauguma šioje disertacijoje tyrinėjamų objektų priklauso šiai Cefėjo atšakai. Šio darbo tikslas yra Cefėjo žvaigždėdaros rajonų, žinomų kaip atspindžio ūkas NGC 7023, tamsiųjų debesų kompleksas TGU 619 ir jaunas spiečius NGC 7129 fotometrinis tyrimas, siekiant nustatyti šių objektų nuotolį ir tarpžvaigždinę ekstinkciją, jauno spiečiaus NGC 7129 ir... [toliau žr. visą tekstą]
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Juárez, Rodríguez Carmen. "Collapse scenarios in magnetized star-forming regions." Doctoral thesis, Universitat de Barcelona, 2017. http://hdl.handle.net/10803/459253.

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Turbulence, magnetic fields and gravity driven flows are important for the formation of new stars. Although magnetic fields have been proven to be important in the formation of stars, only a few works have been done combining magnetic field and kinematic information. Such studies are important to analyze both gravity and gas dynamics and be able to compare them with the magnetic field. In this thesis we will combine dust polarization studies with kinematic analysis towards different star-forming regions. We aim to study the physical properties at core scales (<0.1 pc) from molecular line and dust emission, and study the role of the magnetic field in their dynamic evolution. For this, we will use millimeter and submillimeter observational data taken towards low- and high- mass star-forming regions in different environments and evolutionary states. The first project is the study of the physical, chemical and magnetic properties of the pre-stellar core FeSt1-457 in the Pipe nebula. We studied the emission of the molecular line N2H+(1-0) which is a good tracer of dense gas and therefore describes well the structure of the core. In addition, we detected more than 15 molecular lines and found a clear chemical spatial differentiation for molecules with nitrogen, oxygen and sulfur. Using the ARTIST radiative transfer code (Brinch & Hogerheijde 2010, Padovani et al., 2011, 2012, Jørgensen et al., 2014), we simulated the emission of the different molecules detected and estimated their abundance. In addition, we estimated the magnetic field properties of the core (using the Chandrasekhar-Fermi approximation) from polarization data previously obtained by Alves et al., (2014). Finally, we found interesting correlations between the polarization properties and the chemistry in the region. The second project is the study of a high-mass star-forming region called NGC6334V. NGC6334V is in a more advanced evolutionary state and in an environment surrounded by other massive star-forming regions. During the project we studied the magnetic field from the polarized emission of the dust and also the kinematics of the gas from the molecular line emission of the different tracers of dense gas. From the molecular emission of the gas tracing the envelope of the dense core, we see two different velocity structures separated by 2 km/s and converging towards the potential well in the region. In addition, the magnetic field also presents a bimodal pattern following the distribution of the two velocity structures. Finally, we compared the observational results with 3D magnetohydrodynamic simulations of star-forming regions dominated by gravity. The last project is the study of a lower-mass star-forming region, L1287. From the data obtained with the SMA, the dust continuum structure shows six main dense cores with masses between ~0.4 and 4 solar masses. The dense gas tracer DCN(3-2) shows two velocity structures separated by 2-3 km/s, converging towards the highest-density region, the young stellar object IRAS00338+6312, in a similar scenario to the one observed in the higher-mass case of NGC6334V. Finally, the studies of the pre-stellar core FeSt1-457 and the massive region NGC6334V, show how the magnetic field has been overcome by gravity and is not enough to avoid the gravitational collapse. In addition, NGC6334V and the lower- mass region L1287 present very similar scenarios with the material converging from large scales (~0.1 pc) to the potential wells of both regions at smaller scales (~0.02 pc) through two dense gas flows separated by 2-3 km/s. In a similar scenario, FeSt1-457 is located just in the region where two dense gas structures separated by 3 km/s appear to converge.
La turbulencia, el campo magnético y la gravedad juegan un papel importante en la formación estelar. Aunque se ha mostrado que el campo magnético es importante, sólo se han llevado a cabo un número limitado de trabajos combinando el estudio del campo magnético y la cinemática del gas. Este tipo de trabajos son esenciales para estudiar la gravedad y la dinámica del gas y poder compararlas con el campo magnético a las mismas escalas espaciales. En este trabajo combinamos estudios de polarización a partir de la emisión del polvo, con el análisis de la cinemática del gas en diferentes regiones de formación estelar. El objetivo es estudiar las propiedades físicas a escalas de núcleos densos (<0.1 pc) a partir de la emisión molecular y del polvo, y estudiar el papel del campo magnético en la evolución dinámica de las regiones. Para ello hemos utilizado datos observacionales milimétricos y submilimétricos. Los estudios se han realizado en 3 regiones de formación estelar. El núcleo pre- estelar FeSt 1-457 localizado en un entorno aislado y muy magnetizado en la nebulosa de la Pipa. NGC 6334 V, una región de mayor masa, en un estado evolutivo más avanzado y en un entorno rodeado de otras regiones de formación estelar masiva. Y L1287, una región menos masiva pero con características similares a NGC 6334 V, con presencia de gas de alta velocidad y fuentes centimétricas e infrarrojas. Los estudios del núcleo pre-estelar FeSt 1-457 y la región de formación estelar de alta masa NGC 6334 V, muestran como el campo magnético ha sido superado por la gravedad y no es suficiente para evitar el colapso gravitatorio. Además NGC 6334 V y la región de menor masa L1287 presentan escenarios muy similares, con el material convergiendo desde escalas grandes hacia los pozos de potencial de ambas regiones a escalas más pequeñas a través de flujos de gas denso separados por 2-3 km/s. En un escenario parecido, FeSt 1-457 se encuentra justo en la zona donde parecen converger dos flujos de gas denso separados por 3 km/s.
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Simon, Robert. "Multiline CN observations of star forming regions." [S.l. : s.n.], 1997. http://deposit.ddb.de/cgi-bin/dokserv?idn=955972264.

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Books on the topic "Star-forming"

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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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Torres, Diego F., and Olaf Reimer, eds. Cosmic Rays in Star-Forming Environments. Berlin, Heidelberg: Springer Berlin Heidelberg, 2013. http://dx.doi.org/10.1007/978-3-642-35410-6.

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D, Kunth, Trinh Xuan Thuan, and Tran J. Thanh Van, eds. Star-forming dwarf galaxies and related objects. Gif sur Yvette, France: Frontieres, 1985.

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Cowley, William. The Nature of Dusty Star-Forming Galaxies. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-66748-5.

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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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Workshop on Star-Forming Dwarf Galaxies and Related Objects (1985 Institut d'Astrophysique, Paris). Proceedings of the Workshop on Star-Forming Dwarf Galaxies and related objects, July 1-3, 1985, Institut d'Astrophysique, Paris, France. [Paris]: Editions Frontieres, 1986.

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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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Strickland, David Kendal. X-ray emission from starburst-driven galactic winds: A confrontation between the theory and observations of the violent interstellar medium in star forming galaxies. Birmingham: University of Birmingham, 1998.

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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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Book chapters on the topic "Star-forming"

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Schulz, Norbert S. "Star-Forming Regions." In The Formation and Early Evolution of Stars, 293–322. Berlin, Heidelberg: Springer Berlin Heidelberg, 2012. http://dx.doi.org/10.1007/978-3-642-23926-7_11.

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Wilking, B. A., L. G. Mundy, and R. D. Schwartz. "The Circumstellar Environment of LkHα 234." In Star Forming Regions, 368. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_115.

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Di Fazio, A. "A New Theory of Star Formation: Analytical Mass Function and Star Formation Rate." In Star Forming Regions, 442–43. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_143.

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Shuter, W. L. H., R. L. Dickman, and C. Klatt. "21 cm Line Study of Large Scale Density Fluctuations in the Taurus Molecular Complex." In Star Forming Regions, 67–68. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_15.

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Tomisaka, Kohji. "Formation of Giant Molecular Clouds by Coagulation of Small Molecular Clouds in a Spiral Gravitational Potential." In Star Forming Regions, 541–43. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_160.

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Wynn-Williams, C. G. "Bursts of Star Formation in Galaxies." In Star Forming Regions, 587–97. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_172.

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García-Barreto, J. A., and P. Pişmiş. "Radio Continuum Observations of the Barred Galaxy NGC 4314." In Star Forming Regions, 626–27. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_183.

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Rengarajan, T. N., and R. P. Verma. "FIR and Blue Luminosities and Gas Mass in Spiral Galaxies." In Star Forming Regions, 657–58. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_203.

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Saito, Shuji. "Laboratory Microwave Spectroscopy of Interstellar Molecules." In Star Forming Regions, 92. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_33.

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Tomita, Yoshio. "Observation of the Large Scale Structures of Dark Clouds." In Star Forming Regions, 51–55. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4782-5_6.

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Conference papers on the topic "Star-forming"

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Charnley, S. B. "Chemistry of star-forming cores." In The 50th international meeting of physical chemistry: Molecules and grains in space. AIP, 1994. http://dx.doi.org/10.1063/1.46622.

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Kelm, Birgit. "Single Star-Forming Galaxies and Star-Forming Galaxies in SF + SF and Mixed Pairs." In THE EVOLUTION OF STARBURSTS: The 331st Wilhelm and Else Heraeus Seminar. AIP, 2005. http://dx.doi.org/10.1063/1.2034966.

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Lisitsin, D. D., and A. V. Kuzin. "Identification of extragalactic star forming complexes." 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/b978-5-7996-3229-8.08.

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We developed a technique for selecting star forming complexes in external galaxies based on an analysis of radiation maps in various spectral bands. Using this method, we identified star formation complex candidates in 17 nearby galaxies applying three criteria. These criteria are polycyclic aromatic hydrocarbon emission, dust emission, and ultraviolet young star emission. Relating the information derived from these criteria, we made a sample of star forming regions suitable for revealing correlations between various star formation tracers.
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Porter, Troy. "Cosmic rays in star-forming galaxies." In CENTENARY SYMPOSIUM 2012: DISCOVERY OF COSMIC RAYS. AIP, 2013. http://dx.doi.org/10.1063/1.4792557.

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Padoan, P., A. G. Kritsuk, T. Lunttila, M. Juvela, A. Nordlund, M. L. Norman, S. D. Ustyugov, et al. "MHD Turbulence In Star-Forming Clouds." In PLASMAS IN THE LABORATORY AND THE UNIVERSE: Interactions, Patterns, and Turbulence. AIP, 2010. http://dx.doi.org/10.1063/1.3460128.

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Gerssen, Joris, David Wilman, Lise Christensen, Victor P. Debattista, and C. C. Popescu. "Mapping Star Forming & AGN Galaxies." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458498.

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Pierrick, Martin. "Cosmic Rays in star forming galaxies." In Cosmic Rays and the InterStellar Medium. Trieste, Italy: Sissa Medialab, 2015. http://dx.doi.org/10.22323/1.221.0018.

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Romero, Gustavo E., Felix A. Aharonian, Werner Hofmann, and Frank Rieger. "Gamma rays from star-forming regions." In HIGH ENERGY GAMMA-RAY ASTRONOMY: Proceedings of the 4th International Meeting on High Energy Gamma-Ray Astronomy. AIP, 2008. http://dx.doi.org/10.1063/1.3076825.

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Caillault, Jean-Pierre. "Stellar clusters and star-forming regions." In The soft x-ray cosmos: ROSAT science symposium and data analysis workshop. AIP, 1994. http://dx.doi.org/10.1063/1.46667.

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Wiebe, Dmitry. "Dust in Star Forming Regions - A Review." In Frontier Research in Astrophysics – II. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.269.0023.

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Reports on the topic "Star-forming"

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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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Hidetoshi, Sano. Star Forming Dense Cloud Cores in the TeV -ray SNR RX J1713.7-3946. Office of Scientific and Technical Information (OSTI), October 2010. http://dx.doi.org/10.2172/993416.

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Riveros, Guillermo, Felipe Acosta, Reena Patel, and Wayne Hodo. Computational mechanics of the paddlefish rostrum. Engineer Research and Development Center (U.S.), September 2021. http://dx.doi.org/10.21079/11681/41860.

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Purpose – The rostrum of a paddlefish provides hydrodynamic stability during feeding process in addition to detect the food using receptors that are randomly distributed in the rostrum. The exterior tissue of the rostrum covers the cartilage that surrounds the bones forming interlocking star shaped bones. Design/methodology/approach – The aim of this work is to assess the mechanical behavior of four finite element models varying the type of formulation as follows: linear-reduced integration, linear-full integration, quadratic-reduced integration and quadratic-full integration. Also presented is the load transfer mechanisms of the bone structure of the rostrum. Findings – Conclusions are based on comparison among the four models. There is no significant difference between integration orders for similar type of elements. Quadratic-reduced integration formulation resulted in lower structural stiffness compared with linear formulation as seen by higher displacements and stresses than using linearly formulated elements. It is concluded that second-order elements with reduced integration and can model accurately stress concentrations and distributions without over stiffening their general response. Originality/value – The use of advanced computational mechanics techniques to analyze the complex geometry and components of the paddlefish rostrum provides a viable avenue to gain fundamental understanding of the proper finite element formulation needed to successfully obtain the system behavior and hot spot locations.
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