Proteome analysis of high affinity mouse saliva proteins to hydroxyapatite

Ohshima, Keijiro; Ohshima, Tomoko; Meyer, Karen; Takai, Eisuke; Yoshizawa, Shunsuke; Shiraki, Kentaro; Maeda, Nobuyo

doi:10.1016/j.heliyon.2022.e10077

Cited by 4 publications

(3 citation statements)

References 34 publications

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“…Standstills, which have been observed in ER UMa types for short-period dwarf novae, are intermediate phases following an outburst peak with flat brightness that is about 0.7 mag fainter than the peak brightness (Buat-Ménard et al 2001b;Szkody et al 2013). Their duration ranges from as short as a few weeks to as large as more than a year (Ohshima 2022). During the multiple outbursts O1-O6, the brightness of KSP-OT-201712a stalls at intermediate magnitudes of about two days that are 0.8-1 mag fainter than the peak magnitudes after each outburst peak, consistent with the behavior of short-interval standstills observed in other ER UMa-type dwarf novae.…”

Section: The Nature Of Ksp-ot-201712a and Its Outburstsmentioning

confidence: 93%

Section: The Nature Of Ksp-ot-201712a and Its Outburstsmentioning

confidence: 99%

“…Standstills, which have been observed in ER UMa types and its long-period version of Z Cam types, are known to be caused by a large mass-transfer rate (Buat-Ménard et al 2001b;Ohshima 2022). However, a dwarf nova with a cluster of recurring standstills (as seen in the O1-O6 period of KSP-OT-201712a), maintaining the minimum brightness substantially above the quiescent level, is extremely rare because dwarf novae return to a quiescent phase after a standstill (Ohshima 2022). Even in the case of the few dwarf novae that show a standstill followed by an outburst activity instead of immediately returning to a quiescent phase (Simonsen 2011;Szkody et al 2013;Kato et al 2019;Kato 2019), the outburst activity is very simple and composed of a single outburst.…”

Section: The Nature Of Ksp-ot-201712a and Its Outburstsmentioning

confidence: 99%

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Helium-deficient ER UMa-type Dwarf Nova below the Period Minimum with a Hot Secondary

Lee,

Moon,

Kim

et al. 2024

ApJ

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We present the discovery of a peculiar dwarf nova KSP-OT-201712a using high-cadence, multicolor observations made with the Korea Microlensing Telescope Network. KSP-OT-201712a exhibits a rare presence of outbursts during standstills, as well as strong Hα emission for a dwarf nova below the period minimum with an orbital period of 58.75 ± 0.02 minutes. The outburst cycles are ∼6.6 days within standstills but increase to ∼15 days outside of them. Both B − V and V − I colors become bluer and redder as the outburst luminosities increase and decrease, respectively, for the outburst within standstill, while they evolve in the opposite directions outside of the standstills. The presence of strong double-peaked Hα and weak He i emission lines with He/H flux ratio of 0.27, together with absorption lines of Mg b and Na D in the source, leads to the estimation T eff ≃ 4570 ± 40 K, [Fe/H] ≃ 0.06 ± 0.15 dex, and log g ≃ 4.5 ± 0.1 for its secondary. KSP-OT-201712a is the second He-deficient dwarf nova below the period minimum, while the temperature of the secondary is measured for the first time in such objects. We identify it to be an ER UMa-type dwarf nova, suggesting that the evolution of dwarf novae across the period minimum is accompanied by large mass transfers. The high temperature of the secondary indicates that the system started its mass transfer when the secondary was about 93% of its main-sequence age. The system will evolve to a helium cataclysmic variable or to AM CVn once its hydrogen envelope is exhausted before it explodes as a Type Ia supernova.

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Section: The Nature Of Ksp-ot-201712a and Its Outburstsmentioning

confidence: 93%