Thorne and Zytkow and others hypothesised that, when a neutron star sinks inside another star, a stable star like object would be formed. For decades astronomers have been trying to unambiguously detect this exotic object. Several suggestions were made. By far the most promising candidate appeared to be a red luminous star located in the southern sky HV 2112, as pointed out by Emily Levesque. The star shows evidence for having a strange chemical composition and, if indeed located in the Small Magelanic Cloud, would have been extraordinarily bright.
We show that the object has a large proper motion, meaning that it should be located much closer in the fore ground. If this measurement is robust, it would exclude its TZO nature. To explain the abundance patterns we propose a standard binary scenario for extrinsic S stars. Here, the Mo and Rb came from the wind of a former AGB binary companion, Li is made in situ by the star itself as it rises to it’s own AGB phase. The Ca and K composition are naturally explained by this scenario where the star is part of the very old galactic Halo, where alpha enhanced compositions are normal.
Core-collapse supernovae (SNe) are among the most powerful explosions in the Universe. They mark the deaths of massive stars, most of which are thought to spend their life with in close binary systems. Twenty years after the explosion SN 1994I, long considered to be the result of a binary system, we use Hubble to search for a companion. No companion was detected. We derive deep upper limits in the ultra violet, which allow us to exclude the presence of a main sequence companion with a mass > 10M⊙
We compare with extensive simulations conducted by Manos Zapartas and show that the new data excludes interacting binaries with semi-conservative (late Case A or early Case B) mass transfer. The limits tend to favor systems with non-conservative, late Case B mass transfer with intermediate initial orbital periods and mass ratios. The most likely mass range for a putative main sequence companion would be ∼5–12M⊙, the upper end of which corresponds to the inferred upper detection limit.
Results will be published in the Astrophysical Journal, by Van Dyk, de Mink and Zapartas, 2016.
Using ESO’s Very Large Telescope, an international team of astronomers have found the hottest and most massive double star with components so close that they touch each other. The two stars in the extreme system VFTS 352 could be heading for a dramatic end, during which the two stars either coalesce to create a single giant star, or form a binary black hole.
Almeida, Sana, de Mink et al. ApJ in press, preprint
De Mink & Belcynski, (2015, accepted for publication in ApJ)
With the advanced Gravitational Wave detectors coming online, astrophysicists hope to soon detect the signal from the merger of two neutron stars (NS) or black holes (BH). We investigate the impact of the new constraints on the birth properties of massive stars on the predicted rates for NS and BH mergers. Despite the large changes with previous assumptions (larger binary fraction, stronger preference for very tight systems), we only find an increase of less than a factor 2 (insignificant compared with evolutionary uncertainties of typically a factor 10-100). The uncertainties do not significantly affect (within a factor of 2) our predictions of double compact object merger rates. An exception is the uncertainty in IMF (variations by a factor of 6 up and down). No significant changes in the distributions of final component masses, mass ratios, chirp masses and delay times are found. We conclude that the predictions are, for practical purposes, robust against uncertainties in the initial conditions concerning binary parameters with exception of the IMF. This eliminates an important layer of the many uncertain assumptions affecting the predictions of merger detection rates with the gravitational wave detectors aLIGO/aVirgo.
We explore a newly proposed channel to create binary black holes of stellar origin. This scenario applies to massive, tight binaries where mixing induced by rotation and tides transports the products of hydrogen burning throughout the stellar envelopes. This slowly... Read more »
The Tarantula nebula is a region of extreme star formation located in a satellite galaxy of our milky way. Sabbi and the HTTP team present the results from a treasure survey conducted with the Hubble Space Telescoope identifying the brightness, colors and positions of 800,000 sources, going down to subsolar masses. For this Hubble took images in 8 different filters from the near ultra violet to the near infrared
The HTTP catalogue is the richest sample of intermediate and low mass pre-main sequence candidates. It allows to study how star formation has been developing through the region and the dual role stellar feedback in quenching and triggering star formation. The results have been accepted for publication in ApJS.
Hubble Tarantula Treasury Project. III. Photometric Catalog and Resulting Constraints on the Progression of Star Formation in the 30 Doradus Region by E. Sabbi, D.J. Lennon, J. Anderson, M. Cignoni, R.P. van der Marel, D. Zaritsky, G. de Marchi, N. Panagia, D.A. Gouliermis, E.K. Grebel, J.S. Gallager III, L.J. Smith, H. Sana, A. Aloisi, M. Tosi1, C.J. Evans, H. Arab, M. Boyer, S.E. de Mink, K. Gordon, A.M. Koekemoer, S.S. Larsen, J.E. Ryon, P. Zeidler
Most star clusters at an intermediate age (1-2 Gyr) in the Magellanic Clouds show a puzzling feature in their color-magnitude diagrams. The main sequence turn-off of these clusters is much broader than expected. One (highly-debated) interpretation of this feature is that age spreads of the order 200-500 Myr exist within individual clusters.
We analyze 12 clusters that show an extended turn-off using data taken with the Hubble Telescope. We fit the star formation history of the turn-off and the red clump independently with two different models. In most of the cases, the age spreads inferred from the red clumps are smaller than the ones resulting from the turn-off region. The width of the main sequence turn-off feature is correlated with the age of the clusters in a way which would be unexplained in the “age spread” interpretation, but which may be expected if stellar rotation is the cause of the spread at the turn-off.
F. Niederhofer, N. Bastian, V. Kozhurina-Platais, M. Hilker, S. E. de Mink, I. Cabrera-Ziri, C. Li, B. Ercolano, “Controversial Age Spreads from the Main Sequence Turn-Off and Red Clump in Intermediate-Age Clusters in the LMC”, accepted for publication in A&A
Oxygen Wolf-Rayet (WO) stars represent a very rare late stage in the evolution of massive stars. Their spectra show strong emission lines of helium-burning products, in particular highly ionized carbon and oxygen. They can teach us about the final evolutionary stages of massive stars as they are on the verge of exploding as supernovae.
We use the X-Shooter instrument on the Very Large Telescope in Chili investigate several WO stars. We find that the stars are extremely hot, 150 kK to 210 kK, more than 100,000 times brighter than the sun, with surfaces rich in oxygen and carbon (helium mass fractions less than 44% -14%). They lose mass at a rate that is 2-3 times higher than predicted.
We conclude that WO stars indeed represent the final evolutionary stage of very massive star that start their live with masses of about 40−60M⊙. They are in their final evolutionary stages (post core-helium burning) and predicted to explode as “type Ic supernovae” within just a few thousand years.
Tramper et al. (2015), Accepted for publication in Astronomy & Astrophysics.
The nearby dwarf starburst galaxy NGC5253 hosts a number of young, massive star clusters, the two youngest of which are centrally concentrated and surrounded by thermal radio emission.
To investigate the role of these clusters in the starburst energetics, we use Hubble Space Telescope images of NGC5253 combined with data of the Treasury Program LEGUS (Legacy Extragalactic UV Survey). The extraordinarily well-sampled spectral energy distributions enable modeling with unprecedented accuracy the ages, masses, and extinctions of the brightest clusters.The clusters have ages ~1-15 Myr and masses ~10,000 – 250,000 solar masses.
The most massive cluster is in the radio nebula; with a mass 250,000 solar masses and an age ~1 Myr, 2-4 times less massive and younger than previously estimated. The second radio nebula cluster is also ~1 Myr old, confirming the extreme youth of the starburst region. These two clusters account for about half of the ionizing photon rate in the radio nebula, and will eventually supply about 2/3 of the mechanical energy in present-day shocks. Additional sources are required to supply the remaining ionizing radiation, and may include very massive stars.
Calzetti & the LEGUS collaboration (2015), Accepted for publication in the Astrophysical Journal,
The star cluster Westerlund 2 is one of the most massive young star clusters known in the Milky Way. New data taken with the Hubble Space Telescope allowed Peter Zeidler to study the very young low mass stars in the dense center. These low mass stars are so young that they have not even started nuclear fusion in their center and still reside on the pre main sequence. Surprisingly two clumps were found with an age of less than 2 Myr.
This data of this program was used for Hubble’s 25th birthday image. Zeidler et al. (2015), published in AJ.