We model and analyze the secular evolution of stellar bars in spinning dark matter (DM) haloes with the cosmological spin λ ∼ 0 − 0.09. Using high-resolution stellar and DM numerical simulations, we focus on angular momentum exchange between stellar discs and DM haloes of various axisymmetric shapes -spherical, oblate and prolate. We find that stellar bars experience a diverse evolution which is guided by the ability of parent haloes to absorb angular momentum, J, lost by the disc through the action of gravitational torques, resonant and non-resonant. We confirm that dynamical bar instability is accelerated via resonant J-transfer to the halo. Our main findings relate to the long-term, secular evolution of disc-halo systems: with an increasing λ, bars experience less growth and basically dissolve after they pass through vertical buckling instability. Specifically, with increasing λ, (1) The vertical buckling instability in stellar bars colludes with inability of the inner halo to absorb J -this emerges as the main factor weakening or destroying bars in spinning haloes; (2) Bars lose progressively less J, and their pattern speeds level off; (3) Bars are smaller, and for λ > ∼ 0.06 cease their growth completely following buckling; (4) Bars in λ > 0.03 halos have ratio of corotation-to-bar radii, R CR /R b > 2, and represent so-called slow bars without offset dust lanes. We provide a quantitative analysis of J-transfer in disc-halo systems, and explain the reasons for absence of growth in fast spinning haloes and its observational corollaries. We conclude that stellar bar evolution is substantially more complex than anticipated, and bars are not as resilient as has been considered so far.
The transcription factor Ets2 has a role in cancer development and represents an attractive therapeutic target. In this study, we designed a triplex-forming oligonucleotide (TFO) directed to a homopurine:homopyrimidine sequence in the Ets2 promoter. Transcription factors of the Sp family bound to this sequence and mutation of the Sp1 site reduced Ets2 promoter activity. The Ets2-TFO had high binding affinity for the target sequence and inhibited binding of Sp1/Sp3 to the overlapping site. This effect occurred with a high degree of sequence specificity. Mismatched oligonucleotides did not inhibit Sp1/Sp3 binding and mutations in the target sequence that abolished triplex formation prevented inhibition of Sp1/Sp3 binding by the TFO. The Ets2-TFO inhibited Ets2 promoter activity and expression of the endogenous gene in prostate cancer cells at nanomolar concentrations. The TFO did not affect reporter constructs with mutations in the TFO binding site and promoters of non-targeted genes. Expression of non-targeted genes was also not affected in TFO-treated cells. Collectively, these data demonstrated that the anti-transcriptional activity of the Ets2-TFO was sequence- and target-specific, and ruled out alternative, non-triplex mediated mechanisms of action. This anti-transcriptional approach may be useful to examine the effects of selective downregulation of Ets2 expression and may have therapeutic applications.
We study non-linear response of spinning dark matter (DM) haloes to dynamic and secular evolution of stellar bars in the embedded galactic discs, using high-resolution numerical simulations. For a sequence of haloes with the cosmological spin parameter λ = 0–0.09, and a representative angular momentum distribution, we analyse evolution of induced DM bars amplitude and quantify parameters of the response as well as trapping of DM orbits and angular momentum transfer by the main and secondary resonances. We find that (1) maximal amplitude of DM bars depends strongly on λ, while that of the stellar bars is indifferent to λ; (2) efficiency of resonance trapping of DM orbits by the bar increases with λ, and so is the mass and the volume of DM bars; (3) contribution of resonance transfer of angular momentum to the DM halo increases with λ, and for larger spin, the DM halo ‘talks’ to itself, by moving the angular momentum to larger radii – this process is maintained by resonances; and (4) prograde and retrograde DM orbits play different roles in angular momentum transfer. The ‘active’ part of the halo extends well beyond the bar region, up to few times the bar length in equatorial plane and away from this plane. (5) We model evolution of discless DM haloes and haloes with frozen discs, and found them to be perfectly stable to any Fourier modes. Finally, further studies adopting a range of mass and specific angular momentum distributions of the DM halo will generalize the dependence of DM response on the halo spin and important implications for direct detection of DM and that of the associated stellar tracers, such as streamers.
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