Search Results - "main-sequence star"

The face-on disc of MAXI J1836-194 by Russell, Thomas, Soria, Roberto, Motch, C., Pakull, M., Torres, M., Curran, Peter, Jonker, P., Miller-Jones, James

“…The donor is a main-sequence star with a mass <0.65 M and a radius <0.59 R with an orbital period of <4.9 h. …”
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The detectability of radio emission from exoplanets by Lynch, Christene, Murphy, T., Lenc, E., Kaplan, D.

“…We report new estimates for the radio flux densities and maximum emission frequencies for the current population of known exoplanets orbiting pre-main-sequence and main-sequence stars with spectral types F-M. The set of exoplanets predicted to produce observable radio emission are Hot Jupiters orbiting young stars. …”
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Rapid evolution of the recurrence time in the repeating partial tidal disruption event eRASSt J045650.3-203750 by Liu, Z., Ryu, T., Goodwin, Andrew, Rau, A., Homan, D., Krumpe, M., Merloni, A., Grotova, I., Anderson, Gemma, Malyali, A., Miller-Jones, James

“…Our hydrodynamic simulations suggest that, in the repeating pTDE scenario, such a rapid evolution of Trecur could be reproduced if the original star is a 1 M⊙ main sequence star near the terminal age, losing nearly 80- 90% of its mass during the initial encounter with a supermassive black hole (SMBH) of a mass around 105 M⊙. …”
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Clustering properties of BzK-selected galaxies in goods-N: Environmental quenching and triggering of star formation at z ~ 2 by Lin, L., Dickinson, M., Jian, H., Merson, A., Baugh, C., Scott, D., Foucaud, S., Wang, W., Yan, C., Yan, H., Cheng, Y., Guo, Y., Helly, J., Kirsten, Franz, Koo, D., Lagos, C., Meger, N., Messias, H., Pope, A., Simard, L., Grogin, N., Wang, S.

“…On the other hand, the clustering dependence on SSFR changes abruptly at 2 × 10-9yr-1, which is the typical value for "main-sequence" star-forming galaxies at z ~ 2. We show that the correlation length reaches a minimum at this characteristic value, and is larger for galaxies with both smaller and larger SSFRs; a dichotomy that is only marginally implied from the predictions of the semi-analytical models. …”
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VALES: III. The calibration between the dust continuum and interstellar gas content of star-forming galaxies by Hughes, T.M., Ibar, E., Villaneuva, V., Aravena, M., Baes, M., Bourne, N., Cooray, A., Davies, L.J.M., Driver, S., Dunne, L., Dye, S., Eales, S., Furlanetto, C., Herrera-Camus, R., Ivison, R.J., van Kampen, E., Lara-Lopez, M.A., Maddox, S., Michałowski, M.J., Oteo, I., Smith, D., Smith, M.W.L., Valiante, E., van der Werf, Paul, Viaene, S., Xue, Y.Q.

“…We present the calibration between the dust continuum luminosity and interstellar gas content obtained from the Valparaiso ALMA Line Emission Survey (VALES) sample of 67 main-sequence star-forming galaxies at 0.02 < z < 0.35. …”
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The mean star formation rates of unobscured QSOs: searching for evidence of suppressed or enhanced star formation by Stanley, F., Alexander, D.M., Harrison, C.M., Rosario, D.J., Wang, L., Aird, J.A., Bourne, N., Dunne, L., Dye, S., Eales, S., Knudsen, K.K., Michałowski, M.J., Valiante, E., De Zotti, G., Furlanetto, C., Ivison, R., Maddox, S., Smith, M.W.L.

“…On the basis of the available virial BH masses, and the evolving BH mass to stellar mass relationship, we find that the mean SFRs of our QSO sample are consistent with those of main sequence star-forming galaxies. Similarly the radio-luminous QSOs have mean SFRs that are consistent with both the overall QSO sample and with star-forming galaxies on the main sequence. …”
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VALES. II. The physical conditions of interstellar gas in normal star-forming galaxies up to z=0.2 revealed by ALMA by Hughes, T.M., Ibar, E., Villanueva, V., Aravena, M., Baes, M., Bourne, N., Cooray, A., Dunne, L., Dye, S., Eales, S., Furlanetto, C., Herrera-Camus, R., Ivison, R.J., van Kampen, E., Lara-Lopez, M.A., Maddox, S.J., Michalowski, M.J., Smith, M.W.L., Valiante, E., van der Werf, P., Xue, Y.Q.

“…We use new Band 3 CO(1–0) observations taken with the Atacama Large Millimeter/submillimeter Array (ALMA) to study the physical conditions in the interstellar gas of a sample of 27 dusty main-sequence star-forming galaxies at 0:03 < z < 0:2 present in the Valparaíso ALMA Line Emission Survey (VALES). …”
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Heating and ionization of the primordial intergalactic medium by high mass x-ray binaries by Knevitt, G., Wynn, G.A., Power, C., Bolton, James S.

“…Using a one-dimensional radiative transfer code, we predict the ionization and temperature profiles surrounding a coeval stellar population, composed of main-sequence stars and HMXBs, at various times after its formation. …”
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An asteroid belt interpretation for the timing variations of the millisecond pulsar b1937+21 by Shannon, Ryan, Cordes, J., Metcalfe, T., Lazio, T., Cognard, I., Desvignes, G., Janssen, G., Jessner, A., Kramer, M., Lazaridis, K., Purver, M., Stappers, B., Theureau, G.

“…Pulsar timing observations have revealed companions to neutron stars that include other neutron stars, white dwarfs, main-sequence stars, and planets. We demonstrate that the correlated and apparently stochastic residual times of arrival from the millisecond pulsar B1937+21 are consistent with the signature of an asteroid belt having a total mass 0.05 M ⊕. …”
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Overview of the Massive Young Star-Forming Complex Study in Infrared and X-ray (MYStIX) project by Feigelson, E., Townsley, L., Broos, P., Busk, H., Getman, K., King, R., Kuhn, M., Naylor, T., Povich, M., Baddeley, Adrian, Bate, M., Indebetouw, R., Luhman, K., McCaughrean, M., Pittard, J., Pudritz, R., Sills, A., Song, Y., Wadsley, J.

“…A catalog of MYStIX Probable Complex Members with several hundred OB stars and 31,784 low-mass pre-main sequence stars is assembled. This sample and related data products will be used to seek new empirical constraints on theoretical models of cluster formation and dynamics, mass segregation, OB star formation, star formation triggering on the periphery of H II regions, and the survivability of protoplanetary disks in H II regions. …”
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Physical and chemical conditions in methanol maser selected hot cores and UCH II regions by Purcell, C., Longmore, S., Burton, M., Walsh, Andrew, Minier, V., Cunningham, M., Balasubramanyam, R.

“…This is likely because the most massive clumps evolve so rapidly that a Hyper-Compact HII or UCHII region is the first visible tracer of star formation.The gas mass to submm/infrared luminosity relation for the combined sample was found to be L ~ M0.68, considerably shallower than expected for massive main-sequence stars. This implies that the mass of the clumps is comparable to, or greater than, the mass of the stellar content.We also find that the mass of the hot core is correlated with the mass of the clump in which it is embedded.…”
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