Journal articles: 'Star formation'

1

Bromm, Volker, and Matthew R. Bate. "Star formation." Physics World 17, no. 10 (October 2004): 25–29. http://dx.doi.org/10.1088/2058-7058/17/10/29.

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Palla, Francesco. "Star Formation." International Astronomical Union Colloquium 120 (1989): 56–67. http://dx.doi.org/10.1017/s0252921100023484.

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Judging from the poster that the Organizing Committee has selected to announce the celebration of Guido Munch Jubilee, one can easily conclude that the main characteristics of the process of star formation as emerged in recent years through the combined efforts of multiwavelengths studies of molecular clouds, were already known, here in Granada, several centuries ago to the masters who built and enriched the enigmatic palace of the Alhambra. As we can appreciate from a quick inspection of the picture, it is rather obvious to infer that stars are the byproduct of a quite complex series of phenomena, each connected to, and somewhat dependent on, the others. Also, stars do not form in isolation, but rather in clusters or associations, with a strong tendency for the largest ones, also the most massive ones, to sit in the middle of the distribution. Moreover, smaller and less massive stars outnumber their massive counterparts, apparently obeying a power-law distribution. Finally, but with the benefit of doubt, it appears that the idea that the whole process reflects an intrinsic fractal nature was also put forward at the time. With this background in mind, let us now turn to the new emerging aspects of the study of star formation.

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Fritze, Uta. "Star cluster formation and star formation: the role of environment and star-formation efficiencies." Astrophysics and Space Science 324, no. 2-4 (November 4, 2009): 129–35. http://dx.doi.org/10.1007/s10509-009-0088-5.

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Hirai, Yutaka, Michiko S. Fujii, and Takayuki R. Saitoh. "SIRIUS project. I. Star formation models for star-by-star simulations of star clusters and galaxy formation." Publications of the Astronomical Society of Japan 73, no. 4 (May 20, 2021): 1036–56. http://dx.doi.org/10.1093/pasj/psab038.

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Abstract Most stars are formed as star clusters in galaxies, which then disperse into galactic disks. Upcoming exascale supercomputational facilities will enable simulations of galaxies and their formation by resolving individual stars (star-by-star simulations). This will substantially advance our understanding of star formation in galaxies, star cluster formation, and assembly histories of galaxies. In previous galaxy simulations, a simple stellar population approximation was used. It is, however, difficult to improve the mass resolution with this approximation. Therefore, a model for forming individual stars that can be used in simulations of galaxies must be established. In this first paper of a series from the SIRIUS (SImulations Resolving IndividUal Stars) project, we demonstrate a stochastic star formation model for star-by-star simulations. An assumed stellar initial mass function (IMF) is randomly assigned to newly formed stars in this model. We introduce a maximum search radius to assemble the mass from surrounding gas particles to form star particles. In this study, we perform a series of N-body/smoothed particle hydrodynamics simulations of star cluster formations from turbulent molecular clouds and ultra-faint dwarf galaxies as test cases. The IMF can be correctly sampled if a maximum search radius that is larger than the value estimated from the threshold density for star formation is adopted. In small clouds, the formation of massive stars is highly stochastic because of the small number of stars. We confirm that the star formation efficiency and threshold density do not strongly affect the results. We find that our model can naturally reproduce the relationship between the most massive stars and the total stellar mass of star clusters. Herein, we demonstrate that our models can be applied to simulations varying from star clusters to galaxies for a wide range of resolutions.

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Tan, Jonathan C. "Massive star and star cluster formation." Proceedings of the International Astronomical Union 2, S237 (August 2006): 258–64. http://dx.doi.org/10.1017/s1743921307001573.

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AbstractI review the status of massive star formation theories: accretion from collapsing, massive, turbulent cores; competitive accretion; and stellar collisions. I conclude the observational and theoretical evidence favors the first of these models. I then discuss: the initial conditions of star cluster formation as traced by infrared dark clouds; the cluster formation timescale; and comparison of the initial cluster mass function in different galactic environments.

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Elmegreen, B. G. "Star Formation During Galaxy Formation." EAS Publications Series 51 (2011): 59–71. http://dx.doi.org/10.1051/eas/1151005.

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Omukai, Kazuyuki. "First Star Formation." Progress of Theoretical Physics Supplement 147 (2002): 129–53. http://dx.doi.org/10.1143/ptps.147.129.

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8

Schaye, Joop. "Star Formation Thresholds." Proceedings of the International Astronomical Union 3, S244 (June 2007): 247–55. http://dx.doi.org/10.1017/s1743921307014056.

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AbstractTo make predictions for the existence of “dark galaxies”, it is necessary to understand what determines whether a gas cloud will form stars. Star formation thresholds are generally explained in terms of the Toomre criterion for gravitational instability. I contrast this theory with the thermo-gravitational instability hypothesis of Schaye (2004), in which star formation is triggered by the formation of a cold gas phase and which predicts a nearly constant surface density threshold. I argue that although the Toomre analysis is useful for the global stability of disc galaxies, it relies on assumptions that break down in the outer regions, where star formation thresholds are observed. The thermo-gravitational instability hypothesis can account for a number of observed phenomena, some of which were thought to be unrelated to star formation thresholds.

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Burrows, Adam. "Protoneutron Star Formation." Publications of the Astronomical Society of Australia 7, no. 4 (1988): 371–81. http://dx.doi.org/10.1017/s1323358000022487.

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AbstractThe theory of neutron star formation is addressed in the light of the detected neutrino burst from SN 1987A. A brief review of how supernova neutrino theory has evolved over the last 30 years and a general analysis of the SN 1987A detections is presented.

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10

Williams, Jonathan P. "Clustered star formation." Proceedings of the International Astronomical Union 1, S227 (May 2005): 128–34. http://dx.doi.org/10.1017/s1743921305004448.

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11

Garay, Guido. "Massive Star Formation." Symposium - International Astronomical Union 221 (2004): 169–80. http://dx.doi.org/10.1017/s0074180900241570.

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The understanding of the formation process of massive stars requires a detailed knowledge of the physical conditions of the cloud environment which is thought to play a critical role in determining the formation mechanism. In recent years there has been a rapid growth of observational and theoretical studies concerning the formation of massive stars. Here I review observational data gathered during the last few years which are providing key evidence concerning the physical processes that take place during the formation of massive stars.

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12

Bodifee, G. "Oscillating Star Formation." Symposium - International Astronomical Union 116 (1986): 397–98. http://dx.doi.org/10.1017/s0074180900149253.

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13

Vogel, Stuart N. "Massive Star Formation." International Astronomical Union Colloquium 140 (1994): 176–84. http://dx.doi.org/10.1017/s0252921100019436.

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AbstractSeveral topics in massive star formation are discussed. These include chemical markers of the evolutionary state of massive protostellar cores, kinematic evidence for gravitational collapse, and studies of massive star formation in different environments.

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14

Elmegreen, B. G. "Triggered Star Formation." EAS Publications Series 51 (2011): 45–58. http://dx.doi.org/10.1051/eas/1151004.

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15

Minkel, JR. "Extreme Star Formation." Scientific American 293, no. 4 (October 2005): 33. http://dx.doi.org/10.1038/scientificamerican1005-33a.

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16

Clarke, C. J., and J. E. Pringle. "Star-disc interactions and binary star formation." Monthly Notices of the Royal Astronomical Society 249, no. 4 (April 15, 1991): 584–87. http://dx.doi.org/10.1093/mnras/249.4.584.

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17

Agarwal, Meghann, and Miloš Milosavljević. "NUCLEAR STAR CLUSTERS FROM CLUSTERED STAR FORMATION." Astrophysical Journal 729, no. 1 (February 7, 2011): 35. http://dx.doi.org/10.1088/0004-637x/729/1/35.

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18

Gribel, Carolina, Oswaldo D. Miranda, and José Williams Vilas-Boas. "Connecting the Cosmic Star Formation Rate with the Local Star Formation." Astrophysical Journal 849, no. 2 (November 7, 2017): 108. http://dx.doi.org/10.3847/1538-4357/aa921a.

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19

Farias, Juan P., Jonathan C. Tan, and Sourav Chatterjee. "Star cluster formation from turbulent clumps. II. Gradual star cluster formation." Monthly Notices of the Royal Astronomical Society 483, no. 4 (December 20, 2018): 4999–5019. http://dx.doi.org/10.1093/mnras/sty3470.

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20

Sakhibov, F., and M. A. Smirnov. "Star Formation Properties of 100 Star Formation Complexes in 20 Galaxies." Symposium - International Astronomical Union 207 (2002): 453–55. http://dx.doi.org/10.1017/s0074180900224182.

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The simultaneous multiple constraints of the IMF and SFR history based on the observed UBV R colours, Lyman continuum fluxes and chemical abundances Z resolve the IMF-SFR ambiguity in 100 extragalctic star formation complexes in 20 galaxies (SFCs). The separate study of SFCs with different SFR history shows links between IMF parameters and observed properties of SFCs as well as local and global properties of a host galaxy. The SFR history depends on the star density of SFCs. Low density regions demonstrate instantaneous starburst, while in high density SFCs extended star formation bursts are detected. Constrained IMF slopes are in a good agreement with direct observations of IMFs in OB associations of the Milky Way and LMC.

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21

Hodapp, Klaus-Werner, John Rayner, and Hua Chen. "Luminosity function, star density, and star formation efficiency in regions of star formation - near infrared observations -." Symposium - International Astronomical Union 147 (1991): 289–92. http://dx.doi.org/10.1017/s0074180900239624.

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Clusters of young stars have been found near a number of compact HII regions. These clusters do not show a turnover in the K-band luminosity and are probably several million years old. In L 1641 only moderate clustering tendency has been observed and many sources show signs of extremely young age.

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Hodapp, Klaus-Werner, John Rayner, and Hua Chen. "Luminosity function, star density, and star formation efficiency in regions of star formation - near infrared observations -." Symposium - International Astronomical Union 147 (1991): 289–92. http://dx.doi.org/10.1017/s0074180900199000.

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Clusters of young stars have been found near a number of compact HII regions. These clusters do not show a turnover in the K-band luminosity and are probably several million years old. In L 1641 only moderate clustering tendency has been observed and many sources show signs of extremely young age.

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23

Lada, Elizabeth A., and João F. Alves. "Observations of Star Formation." Symposium - International Astronomical Union 221 (2004): 3–15. http://dx.doi.org/10.1017/s0074180900241405.

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Star formation is a continuous ongoing process occurring over the lifetime of our Galaxy and the universe. However understanding how stars form from their pre-natal clouds of gas and dust remains a mystery. During the last two decades we have made remarkable progress toward unraveling this mystery mainly due to advances in observational technology especially at infrared and millimeter wavelengths which allow direct observation of the sites of star birth. Such observations suggest that embedded clusters may be the fundamental units of star formation in molecular clouds. Low star formation efficiency and rapid gas dispersal make these clusters disperse to provide the field star population. Consequently embedded clusters provide important laboratories for investigating fundamental issues of star formation within our Galaxy.

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24

Larson, R. B. "Star formation in groups." Monthly Notices of the Royal Astronomical Society 272, no. 1 (January 1, 1995): 213–20. http://dx.doi.org/10.1093/mnras/272.1.213.

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25

Hatchell, J., J. S. Richer, G. A. Fuller, C. J. Qualtrough, E. F. Ladd, and C. J. Chandler. "Star formation in Perseus." Astronomy & Astrophysics 440, no. 1 (August 19, 2005): 151–61. http://dx.doi.org/10.1051/0004-6361:20041836.

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26

Pudritz, Ralph E. "Star formation branches out." Nature 457, no. 7225 (December 31, 2008): 37–39. http://dx.doi.org/10.1038/457037a.

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27

Barton, Elizabeth J., Jacob A. Arnold, Andrew R. Zentner, James S. Bullock, and Risa H. Wechsler. "Isolating Triggered Star Formation." Astrophysical Journal 671, no. 2 (December 20, 2007): 1538–49. http://dx.doi.org/10.1086/522620.

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28

Madau, Piero, and Mark Dickinson. "Cosmic Star-Formation History." Annual Review of Astronomy and Astrophysics 52, no. 1 (August 18, 2014): 415–86. http://dx.doi.org/10.1146/annurev-astro-081811-125615.

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29

Tan, Jonathan C., Mark R. Krumholz, and Christopher F. McKee. "Equilibrium Star Cluster Formation." Astrophysical Journal 641, no. 2 (March 30, 2006): L121—L124. http://dx.doi.org/10.1086/504150.

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30

Hammer, F. "Cosmological star formation history." EAS Publications Series 3 (2002): 71–84. http://dx.doi.org/10.1051/eas:2002046.

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31

McKee, Christopher F., and Eve C. Ostriker. "Theory of Star Formation." Annual Review of Astronomy and Astrophysics 45, no. 1 (September 2007): 565–687. http://dx.doi.org/10.1146/annurev.astro.45.051806.110602.

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32

Klaassen, P. D., J. C. Mottram, S. N. Longmore, G. A. Fuller, F. F. S. van der Tak, and L. Kaper. "High-mass star formation." Astronomy & Geophysics 54, no. 3 (May 22, 2013): 3.33. http://dx.doi.org/10.1093/astrogeo/att083.

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33

Fish, Vincent L. "Masers and star formation." Proceedings of the International Astronomical Union 3, S242 (March 2007): 71–80. http://dx.doi.org/10.1017/s1743921307012604.

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AbstractRecent observational and theoretical advances concerning astronomical masers in star forming regions are reviewed. Major masing species are considered individually and in combination. Key results are summarized with emphasis on present science and future prospects.

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34

Knapen, Johan H., Mauricio Cisternas, and Miguel Querejeta. "Interactions and star formation." Proceedings of the International Astronomical Union 11, S315 (August 2015): 236–39. http://dx.doi.org/10.1017/s1743921316007559.

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AbstractWe investigate the influence of interactions on the star formation by studying a sample of almost 1500 of the nearest galaxies, all within a distance of ~45 Mpc. We define the massive star formation rate (SFR), as measured from far-IR emission, and the specific star formation rate (SSFR), which is the former quantity normalized by the stellar mass of the galaxy, and explore their distribution with morphological type and with stellar mass. We then calculate the relative enhancement of these quantities for each galaxy by normalizing them by the median SFR and SSFR values of individual control populations of similar non-interacting galaxies. We find that both SFR and SSFR are enhanced in interacting galaxies, and more so as the degree of interaction is higher. The increase is, however, moderate, reaching a maximum of a factor of 1.9 for the highest degree of interaction (mergers). The SFR and SSFR are enhanced statistically in the population, but in most individual interacting galaxies they are not enhanced at all. We discuss how those galaxies with the largest SFR and/or SSFR enhancement can be defined as starbursts. We argue that this study, based on a representative sample of nearby galaxies, should be used to place constraints on studies based on samples of galaxies at larger distances.

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35

Goodwin, Simon P. "Star formation simulations: caveats." Proceedings of the International Astronomical Union 5, H15 (November 2009): 793. http://dx.doi.org/10.1017/s1743921310011713.

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AbstractStar formation is such a huge problem, covering such a large range of physical scales and involving so many physical processes, that the results of simulations should always be taken with care.

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36

Clarke, C. J. "Binary Star Formation Simulations." Proceedings of the International Astronomical Union 7, S282 (July 2011): 409–16. http://dx.doi.org/10.1017/s1743921311027955.

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AbstractBinary stars provide an excellent calibration of the success or otherwise of star formation simulations, since the reproduction of their statistical properties can be challenging. Here, I summarise the direction that the field has taken in recent years, with an emphasis on binary formation in the cluster context, and discuss which observational diagnostics are most ripe for meaningful theoretical comparison. I focus on two issues: the prediction of binary mass ratio distributions and the formation of the widest binaries in dissolving clusters, showing how in the latter case the incidence of ultra-wide pairs constrains the typical membership number of natal clusters to be of order a hundred. I end by drawing attention to recent works that include magnetic fields and which will set the direction of future research in this area.

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Rengarajan, T. N., R. P. Verma, and K. V. K. Iyengar. "Star Formation and Supernovae." Symposium - International Astronomical Union 115 (1987): 208–9. http://dx.doi.org/10.1017/s0074180900095577.

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We have searched for associations between supernova remnants (SNR) and IRAS sources. For this purpose we used 117 SNRs from the catalogue of van den Bergh and searched the IRAS Point Source Catalogue for sources associated with SNRs and having a flux density spectrum increasing with wavelength beyond 25 m. For each SNR a square box of area 2 deg2 was searched for sources. The difference between the observed number within the SNR (with 10% radial extension) and the number expected on the basis of source density in the box excluding the SNR itself, was termed the excess. The results are shown in Table 1. There are a few SNRs which show significant excess on an individual basis. The cumulative excess of the rest has a 4 significance. For 58 SNRs with well defined maps, the data in Table 1 show that the significance of excess increases in the shell area. Figure 1 shows the excess as a function of distance to SNR. Also plotted are average excesses for different distance intervals. The increase in excess as distance decreases, strengthens the hypothesis of association with SNR, since at shorter distances, more IRAS sources will be above the threshold of detection.

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Bash, Frank, and Michele Kaufman. "Star Formation in M81." Symposium - International Astronomical Union 115 (1987): 626. http://dx.doi.org/10.1017/s0074180900096571.

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VLA observations of the spiral galaxy M81 in the radio continuum at wavelengths of 6 and 20-cm have been used to check the predictions of the density wave theory. The non-thermal radiation from the arms has been detected and the arms are found to be broader than the predictions of the classical density wave theory. Their width does seem to agree with that predicted by models which take the clumpy nature of the interstellar medium into account. These data are also able to separate giant HII regions from the non-thermal arms. Collaborators have furnished optical Hα data on the HII regions and HI 21-cm data, from the VLA, which will be used to find and measure the location of the HII regions with respect to the spiral shock wave and to measure the visual extinction in the disk of M81.

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39

Shu, F. H. "Molecules in star formation." Symposium - International Astronomical Union 178 (1997): 19–30. http://dx.doi.org/10.1017/s0074180900009219.

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We review current ideas and models in the problem of star formation from molecular cloud cores that are relatively isolated from the influences of other forming stars. We discuss the time scales, flow dynamics, and density and temperature structures applicable to each of the four stages of the entire process: (a) formation of a magnetized cloud core by ambipolar diffusion and evolution to a pivotal state of gravomagneto catastrophe; (b) self-similar collapse of the pivotal configuration and the formation of protostars, disks, and pseudo-disks; (c) onset of a magnetocentrifugally driven, lightly ionized wind from the interaction of an accretion disk and the magnetosphere of the central star, and the driving of bipolar molecular outflows; (d) evolution of pre-main-sequnce stars surrounded by dusty accretion disks. For each of these stages and processes, we consider the characteristics of the molecular diagnostics needed to investigate the crucial aspects of the observational problem.

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40

García-Benito, Rubén, Enrique Pérez, Ángeles I. Díaz, Jesús Maíz Apellániz, and Miguel Cerviño. "Star formation in NGC5471." Astrophysics and Space Science 324, no. 2-4 (September 23, 2009): 337–40. http://dx.doi.org/10.1007/s10509-009-0090-y.

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41

Bianchi, Luciana. "GALEX and star formation." Astrophysics and Space Science 335, no. 1 (February 9, 2011): 51–60. http://dx.doi.org/10.1007/s10509-011-0612-2.

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42

van Breugel, Wil, Chris Fragile, Peter Anninos, and Stephen Murray. "Jet-Induced Star Formation." Symposium - International Astronomical Union 217 (2004): 472–79. http://dx.doi.org/10.1017/s0074180900198225.

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Jets from radio galaxies can have dramatic effects on the medium through which they propagate. We review observational evidence for jet-induced star formation in low (‘FR-I’) and high (‘FR-II’) luminosity radio galaxies, at low and high redshifts respectively. We then discuss numerical simulations which are aimed to explain a jet-induced starburst (‘Minkowski's Object’) in the nearby FR-I type radio galaxy NGC 541. We conclude that jets can induce star formation in moderately dense (10 cm−3), warm (104 K) gas; that this may be more common in the dense environments of forming, active galaxies; and that this may provide a mechanism for ‘positive’ feedback from AGN in the galaxy formation process.

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43

Whitworth, Anthony. "Impulsively triggered star formation." Symposium - International Astronomical Union 208 (2003): 71–80. http://dx.doi.org/10.1017/s0074180900207031.

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I contend that impulsively triggered star formation is at least as important as spontaneous quasistatic star formation regulated by ambipolar diffusion, and probably more so. To support this contention, I describe and discuss SPH simulations of (i) star formation triggered by colliding clouds and expanding nebulae (HII regions, stellar-wind bubbles, and supernova remnants); (ii) violent interactions between protostellar discs and the resulting genesis of binary systems and low-mass companions; and (iii) protostellar collapse induced by a sudden increase in external pressure.

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44

Silk, Joseph, and Colin Norman. "GLOBAL STAR FORMATION REVISITED." Astrophysical Journal 700, no. 1 (July 1, 2009): 262–75. http://dx.doi.org/10.1088/0004-637x/700/1/262.

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45

Schilke, P. "High-Mass Star Formation." EAS Publications Series 75-76 (2015): 227–35. http://dx.doi.org/10.1051/eas/1575046.

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46

Crutcher, Richard M. "What Drives Star Formation?" Astrophysics and Space Science 292, no. 1-4 (2004): 225–37. http://dx.doi.org/10.1023/b:astr.0000045021.42255.95.

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47

Tutukov, A. V. "Star formation in galaxies." Astronomical & Astrophysical Transactions 21, no. 1-3 (January 2002): 137–44. http://dx.doi.org/10.1080/10556790215572.

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48

Hatchell, J., G. A. Fuller, J. S. Richer, T. J. Harries, and E. F. Ladd. "Star formation in Perseus." Astronomy & Astrophysics 468, no. 3 (April 11, 2007): 1009–24. http://dx.doi.org/10.1051/0004-6361:20066466.

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49

Hatchell, J., G. A. Fuller, and J. S. Richer. "Star formation in Perseus." Astronomy & Astrophysics 472, no. 1 (June 26, 2007): 187–98. http://dx.doi.org/10.1051/0004-6361:20066467.

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50

Hatchell, J., and G. A. Fuller. "Star formation in Perseus." Astronomy & Astrophysics 482, no. 3 (March 11, 2008): 855–63. http://dx.doi.org/10.1051/0004-6361:20079213.

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Journal articles on the topic 'Star formation'

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